<?xml version="1.0" encoding="UTF-8"?>
<!DOCTYPE article PUBLIC "-//NLM//DTD JATS (Z39.96) Journal Publishing DTD v1.4 20241031//EN" "JATS-journalpublishing1-4.dtd">
<article xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink" article-type="research-article" dtd-version="1.4" xml:lang="en">
  <front>
    <journal-meta>
      <journal-id journal-id-type="publisher-id">jhepgc</journal-id>
      <journal-title-group>
        <journal-title>Journal of High Energy Physics, Gravitation and Cosmology</journal-title>
      </journal-title-group>
      <issn pub-type="epub">2380-4335</issn>
      <issn pub-type="ppub">2380-4327</issn>
      <publisher>
        <publisher-name>Scientific Research Publishing</publisher-name>
      </publisher>
    </journal-meta>
    <article-meta>
      <article-id pub-id-type="doi">10.4236/jhepgc.2026.124106</article-id>
      <article-id pub-id-type="publisher-id">jhepgc-154234</article-id>
      <article-categories>
        <subj-group>
          <subject>Article</subject>
        </subj-group>
        <subj-group>
          <subject>Physics</subject>
          <subject>Mathematics</subject>
        </subj-group>
      </article-categories>
      <title-group>
        <article-title>Evidence for a Solar System Origin of 3I/ATLAS and Related Small Bodies within World-Universe Cosmology</article-title>
      </title-group>
      <contrib-group>
        <contrib contrib-type="author">
          <contrib-id contrib-id-type="orcid">0000-0002-1033-1837</contrib-id>
          <name name-style="western">
            <surname>Netchitailo</surname>
            <given-names>Vladimir S.</given-names>
          </name>
          <xref ref-type="aff" rid="aff1">1</xref>
        </contrib>
      </contrib-group>
      <aff id="aff1"><label>1</label> Independent Researcher, Livermore, CA, USA </aff>
      <author-notes>
        <fn fn-type="conflict" id="fn-conflict">
          <p>The author declares no conflicts of interest regarding the publication of this paper.</p>
        </fn>
      </author-notes>
      <pub-date pub-type="epub">
        <day>01</day>
        <month>10</month>
        <year>2026</year>
      </pub-date>
      <pub-date pub-type="collection">
        <month>10</month>
        <year>2026</year>
      </pub-date>
      <volume>12</volume>
      <issue>04</issue>
      <fpage>2126</fpage>
      <lpage>2155</lpage>
      <history>
        <date date-type="received">
          <day>14</day>
          <month>04</month>
          <year>2026</year>
        </date>
        <date date-type="accepted">
          <day>25</day>
          <month>09</month>
          <year>2026</year>
        </date>
        <date date-type="published">
          <day>28</day>
          <month>09</month>
          <year>2026</year>
        </date>
      </history>
      <permissions>
        <copyright-statement>© 2026 by the authors and Scientific Research Publishing Inc.</copyright-statement>
        <copyright-year>2026</copyright-year>
        <license license-type="open-access">
          <license-p> This article is an open access article distributed under the terms and conditions of the Creative Commons Attribution (CC BY) license ( <ext-link ext-link-type="uri" xlink:href="https://creativecommons.org/licenses/by/4.0/">https://creativecommons.org/licenses/by/4.0/</ext-link> ). </license-p>
        </license>
      </permissions>
      <self-uri content-type="doi" xlink:href="https://doi.org/10.4236/jhepgc.2026.124106">https://doi.org/10.4236/jhepgc.2026.124106</self-uri>
      <abstract>
        <p>The object formally designated C/2025 N1 (ATLAS) has been widely discussed as a candidate third interstellar object (“3I/ATLAS”) due to its strongly hyperbolic trajectory. In standard celestial mechanics, an interstellar origin is inferred when the original barycentric eccentricity significantly exceeds unity prior to planetary perturbations. This interpretation, however, implicitly assumes that cometary dynamics are governed solely by gravitational forces and conventional outgassing. In this work, we propose an alternative hypothesis: C/2025 N1 (ATLAS) is not interstellar but a Small Solar System Body (SB) originating from the Oort Cloud, consistent with the framework of World-Universe Cosmology (WUC). We argue that its large excess velocity can be explained by a non-gravitational internal acceleration mechanism involving partial conversion of the rotational energy of the nucleus into the translational kinetic energy of the SB. Within WUC, the Universe is structured as a hierarchy of interaction regimes—Macro-world (gravity), Large-world (extremely-weak interaction), Small-world (super-weak interaction), and Micro-world (weak interaction). Previous studies associate Ball Lightning [<xref ref-type="bibr" rid="B1">1</xref>] with SB1 and interpret the Tunguska superbolide [<xref ref-type="bibr" rid="B2">2</xref>] as an SB2 analogue. Extending this hierarchy, we identify C/2025 N1 (ATLAS) as an SB3 object. This model naturally accounts for its extreme hyperbolic excess velocity without invoking an interstellar origin and leads to specific, testable predictions regarding kinematics, activity, and radiation signatures. We compare these predictions with observations of ʻOumuamua, C/2019 Q4 (Borisov), and a growing population of low-albedo asteroids and “dark comets” exhibiting dust-poor outgassing.</p>
      </abstract>
      <kwd-group kwd-group-type="author-generated" xml:lang="en">
        <kwd>World-Universe Cosmology</kwd>
        <kwd>Small Solar System Bodies</kwd>
        <kwd>Non-Gravitational Acceleration</kwd>
        <kwd>Multiworld</kwd>
        <kwd>C/2025 N1 (ATLAS)</kwd>
        <kwd>Internal Energy Conversion</kwd>
      </kwd-group>
    </article-meta>
  </front>
  <body>
    <sec id="sec1">
      <title>1. Introduction</title>
      <p>The Interplanetary Medium comprises the matter and energy filling the Solar System (SS), extending outward to the Heliopause—the boundary where the solar wind is balanced by the surrounding Interstellar Medium (ISM). Measurements by the Voyager spacecraft place this boundary at approximately 120 AU, although its shape is asymmetric, compressed in the direction of solar motion and extended in the polar regions.</p>
      <p>Beyond the Heliopause lies ISM. However, the physical and dynamical extent of SS is not necessarily limited to this boundary. The Oort Cloud, a hypothesized reservoir of icy bodies, likely extends from ~10<sup>3</sup> AU to ~10<sup>5</sup> AU and remains gravitationally bound to the Sun. It is commonly divided into an inner disk-like component and a distant, nearly spherical outer component. Although often described as lying in interstellar space, the Oort Cloud is generally understood to consist of material formed within the early Solar System and later scattered outward by interactions with the giant planets.</p>
      <p>Comets are traditionally classified into short-period (ecliptic) comets with orbits within ~10 AU and long-period comets (LPCs) with highly elongated orbits extending to thousands of AU. LPCs appear nearly isotropic in their arrival directions and are widely attributed to the Oort Cloud.</p>
      <p>The discovery of objects on strongly hyperbolic trajectories—such as ʻOumuamua and C/2019 Q4 (Borisov)—has led to the prevailing interpretation that such bodies originate in the ISM. The designation of C/2025 N1 (ATLAS) as a potential third interstellar object (“3I/ATLAS”) follows this paradigm.</p>
      <p>However, this interpretation rests on a key assumption that hyperbolic motion necessarily implies an extrasolar origin. In this paper, we challenge this assumption. In WUC, the effective radius of SS is estimated to be ~96,000 AU, comparable to the outer extent of the Oort Cloud. From this perspective, the Oort Cloud remains an intrinsic component of SS rather than a transitional boundary to interstellar space.</p>
      <p>We therefore explore an alternative hypothesis: C/2025 N1 (ATLAS) is SB3 whose hyperbolic excess velocity arises from the proposed internal, non-gravitational energy conversion mechanism, removing the need to invoke an interstellar origin.</p>
    </sec>
    <sec id="sec2">
      <title>2. Long-Period Comets</title>
      <p>Astronomical observations since the mid-19<sup>th</sup> century have revealed numerous weakly hyperbolic comets, many of which are interpreted as Oort Cloud objects subsequently perturbed onto escape trajectories. In several well-studied cases, comets initially bound to SS transitioned to unbound orbits following close encounters with giant planets. Notable examples include C/1980 E1 (Bowell) and C/2024 L5 (ATLAS), both of which acquired hyperbolic trajectories through planetary scattering.</p>
      <p>Long-period comets (LPCs) are conventionally defined as bodies with orbital periods exceeding 200 years. A subset—very long-period comets—have orbital periods of millions of years and are believed to originate in the outer Oort Cloud. For example, C/1999 F1 (Catalina) has an orbital period of several million years.</p>
      <p>LPCs exhibit several well-established properties:</p>
      <p>Orbital periods: hundreds of years to millions of yearsDynamical origin: perturbations by passing stars, molecular clouds, and galactic tidesIsotropic distribution: reflecting the spherical structure of the outer Oort CloudPrimitive composition<bold>:</bold> high volatile content, leading to strong activity near the Sun</p>
      <p>Recent surveys have expanded the known population of Oort Cloud comets to several thousand objects, a number expected to grow substantially with the Legacy Survey of Space and Time (LSST). Among these, C/2014 UN271 (Bernardinelli-Bernstein) is the largest known Oort Cloud comet and exhibits activity at unusually large heliocentric distances (see <bold>Table 1</bold>).</p>
      <p>A key observational result is that hyperbolic trajectories are not uncommon among LPCs. In most cases, their weak hyperbolicity can be explained by:</p>
      <p>planetary perturbations (e.g., scattering by Jupiter or Saturn)non-gravitational forces driven by asymmetric outgassing</p>
      <p>However, these mechanisms typically produce only weakly hyperbolic orbits, with eccentricities slightly exceeding unity (<italic>e</italic> ≳ 1). Even in extreme cases such as C/1980 E1 (Bowell), the observed excess velocity remains modest and can be quantitatively explained within standard dynamical frameworks.</p>
      <p>In contrast, C/2025 N1 (ATLAS) exhibits an extraordinarily large eccentricity (<italic>e</italic> ≈ 6.14), far beyond the range achievable through known gravitational or outgassing processes. This places it in a fundamentally different dynamical regime.</p>
      <p>We therefore argue that the distinction between typical hyperbolic comets and C/2025 N1 (ATLAS) is qualitative rather than merely quantitative. Its extreme trajectory strongly suggests the presence of a powerful Non-Gravitational Acceleration (NGA) mechanism. Within the present framework, this behavior is naturally interpreted as the result of internal energy conversion.</p>
    </sec>
    <sec id="sec3">
      <title>3. Hyperbolic Asteroids</title>
      <p>Asteroids are conventionally defined as minor planets—solid bodies larger than meteoroids (≳1 m) that do not exhibit cometary activity. Most reside in the main asteroid belt between Mars and Jupiter and are composed primarily of rock and metal. However, modern observations increasingly reveal a continuum between asteroids and comets rather than a strict dichotomy. </p>
      <p>A hyperbolic asteroid is a small body observed on an orbit with eccentricity<italic>e</italic> &gt; 1, implying that it is not gravitationally bound to the Sun. Unlike comets, such objects initially show no detectable coma or outgassing, and their motion appears consistent with purely gravitational dynamics.</p>
      <p><bold>Table 1.</bold> Long-period comets with extreme aphelia.</p>
      <table-wrap id="tbl1">
        <label>Table 1</label>
        <table>
          <tbody>
            <tr>
              <td>
                <bold>Comet</bold>
              </td>
              <td>
                <bold>Inbound Aphelion</bold>
                <bold>(AU)</bold>
                <bold>Orbital</bold>
                <bold>Period</bold>
                <bold>(Myr)</bold>
              </td>
              <td>
                <bold>Outbound Aphelion (AU)</bold>
                <bold>Orbital</bold>
                <bold>Period</bold>
              </td>
            </tr>
            <tr>
              <td>C/1973 E1 (Kohoutek)</td>
              <td>98,000 (~11 Myr)</td>
              <td>3700 (80,000 yr)</td>
            </tr>
            <tr>
              <td>C/1999 F1 (Catalina)</td>
              <td>54,000 (~4 Myr)</td>
              <td>66,000 (~6 Myr)</td>
            </tr>
            <tr>
              <td>C/2000 W1 (Utsunomiya-Jones)</td>
              <td>
                70,000 (Myrs)
                <italic>e</italic>
                = 0.9999996
              </td>
              <td>1670 (~24,000 yr)</td>
            </tr>
            <tr>
              <td>C/2006 P1 (McNaught)</td>
              <td>67,000 (~6 Myr)</td>
              <td>4100 (~92,600 yr)</td>
            </tr>
            <tr>
              <td>C/2010 X1 (Elenin)</td>
              <td>97,000 (Myrs)</td>
              <td>
              </td>
            </tr>
            <tr>
              <td>C/2010 U3 (Boattini)</td>
              <td>34,000 (~2.2 Myr)</td>
              <td>9900 (~350,000 yr)</td>
            </tr>
            <tr>
              <td>C/2011 L4 (PanSTARRS)</td>
              <td>68,000 (Myrs)</td>
              <td>4500 (~107,000 yr)</td>
            </tr>
            <tr>
              <td>C/2013 A1 (Siding Spring)</td>
              <td>52,000 (Several Myr)</td>
              <td>13,000 (~500,000 yr)</td>
            </tr>
            <tr>
              <td>
                C/2014 UN
                <sub>271</sub>
                (Bernardinelli-Bernstein)
              </td>
              <td>
                42,000 (~3 Myr)
                <italic>e</italic>
                = 0.99947
              </td>
              <td>
                59,000 (~5.1 Myr)
                <italic>e</italic>
                = 0.99967
              </td>
            </tr>
            <tr>
              <td>C/2017 K2 (PanSTARRS)</td>
              <td>51,200 (~4.1 Myr)</td>
              <td>1750 (~25,800 yr)</td>
            </tr>
            <tr>
              <td>C/2017 T2 (PanSTARRS)</td>
              <td>74,000 (~7 Myr)</td>
              <td>3000 (~55,000 yr)</td>
            </tr>
            <tr>
              <td>C/2019 E3 (ATLAS)</td>
              <td>65,200 (~5.9 Myr)</td>
              <td>34,000</td>
            </tr>
            <tr>
              <td>C/1980 E1 (Bowell)</td>
              <td>
                75,000 (~7.1 Myr)
                <italic>e</italic>
                = 1.066
              </td>
              <td>
                Oort-cloud comet ejected byJupiter, Hyperbolic,
                <italic>e</italic>
                &gt; 1.057
              </td>
            </tr>
            <tr>
              <td>
                C/2013 US
                <sub>10</sub>
                (Catalina)
              </td>
              <td>38,000 (Several Myr)</td>
              <td>Hyperbolic trajectory</td>
            </tr>
            <tr>
              <td>C/2024 L5 (ATLAS)</td>
              <td>
                Original barycentric
                <italic>e</italic>
                ≈ 0.999
              </td>
              <td>
                Oort-cloud comet ejected by Saturn, Hyperbolic,
                <italic>e</italic>
                &gt; 1.037
              </td>
            </tr>
            <tr>
              <td>C/2023 A3(Tsuchinshan-ATLAS)</td>
              <td>
                ≈380,000 (83 Myr) Originalbarycentric
                <italic>e</italic>
                ≈ 0.999
              </td>
              <td>
                Weakly hyperbolic, Future barycentric
                <italic>e</italic>
                ≈ 1.001 - 1.003
              </td>
            </tr>
            <tr>
              <td>C/2025 N1 (ATLAS)</td>
              <td>
                Original barycentric
                <italic>e</italic>
                &gt; 1.01
              </td>
              <td>
                Ejected by the Sun, strongly hyperbolic trajectory,
                <italic>e</italic>
                = 6.14
              </td>
            </tr>
          </tbody>
        </table>
      </table-wrap>
      <p>In practice, many objects initially classified as hyperbolic asteroids are later reclassified as comets once faint activity is detected. Examples include C/2018 C2 (Lemmon) and C/2018 F4 (PAN-STARRS), both of which exhibited delayed or weak cometary signatures. This highlights the observational challenge of distinguishing inactive comets from asteroids based on early data.</p>
      <p>The most notable confirmed hyperbolic asteroid is ʻOumuamua, which displayed no classical coma yet exhibited significant NGA, likely driven by non-standard outgassing (e.g., H<sub>2</sub> or other low-visibility volatiles).</p>
      <p>A key observational trend is that most hyperbolic small bodies are only weakly unbound, with eccentricities slightly above unity. Their trajectories can generally be explained by:</p>
      <p>gravitational perturbationsradiation pressureweak, often undetected outgassing</p>
      <p>Thus, even among objects classified as asteroidal, strongly hyperbolic trajectories are rare and typically require additional physical explanation.</p>
    </sec>
    <sec id="sec4">
      <title>4. Small Solar System Bodies</title>
      <p>Small Solar System Body is an object in the SS that is neither a planet nor a dwarf planet, nor a natural satellite. The term was first defined in 2006 by the International Astronomical Union as follows: “<italic>All other objects</italic>,<italic>except satellites</italic>, <italic>orbiting the Sun shall be referred to collectively as</italic>‘<italic>Small Solar System Bodies</italic><italic>’</italic>”.</p>
      <sec id="sec4dot1">
        <title>4.1. Dark Comets</title>
        <p>The discovery of ʻOumuamua revealed a new dynamical class of SBs: objects that exhibit NGA without visible cometary activity. Unlike classical comets, ʻOumuamua showed no detectable coma or dust tail, yet its trajectory deviated measurably from a purely gravitational orbit.</p>
        <p>In cometary physics, dust particles are micron- to sub-millimeter-sized solid grains released from the nucleus during volatile sublimation. These grains scatter sunlight and are responsible for the visible coma and dust tail observed in active comets. In contrast, gas species (e.g., H<sub>2</sub>O, CO, H<sub>2</sub>) are dynamically dominant and can produce NGA through anisotropic outgassing. The absence of a detectable dust component, as observed in ʻOumuamua, therefore implies either extremely low dust production or preferential release of gas without entrained solids, consistent with the emerging class of “Dark Comets.”</p>
        <p><bold>Non-Gravitational Acceleration without a Ta</bold><bold>il</bold></p>
        <p>The motion of ʻOumuamua was tracked with high precision using facilities including the Hubble Space Telescope. These observations established that:</p>
        <p>Direction: The excess acceleration was consistently radially outward from the Sun.Magnitude<bold>:</bold> By early 2018, the object was displaced by ~40,000 km from its predicted gravitational trajectory.</p>
        <p>This behavior implies the presence of a continuous, low-level thrust, analogous to cometary outgassing, but without visible ejecta.</p>
        <p><bold>Physical Interpretatio</bold><bold>ns</bold></p>
        <p>Several mechanisms have been proposed to explain this “invisible” acceleration:</p>
        <table-wrap id="tbl2">
          <label>Table 2</label>
          <table>
            <tbody>
              <tr>
                <td>
                  <bold>Mechanism</bold>
                </td>
                <td>
                  <bold>Physical Basis</bold>
                </td>
              </tr>
              <tr>
                <td>Hydrogen outgassing</td>
                <td>
                  Release of trapped H
                  <sub>2</sub>
                  from irradiated ice
                </td>
              </tr>
              <tr>
                <td>Nitrogen ice sublimation</td>
                <td>
                  Evaporation of N
                  <sub>2</sub>
                  from Pluto-like fragments
                </td>
              </tr>
              <tr>
                <td>Radiation pressure</td>
                <td>Momentum transfer from sunlight</td>
              </tr>
              <tr>
                <td>“Dark comet” activity</td>
                <td>Dust-poor water vapor outgassing</td>
              </tr>
            </tbody>
          </table>
        </table-wrap>
        <p>The emerging consensus favors hydrogen outgassing, consistent with an icy body whose surface layers were chemically altered by long-term cosmic-ray exposure in interstellar space.</p>
        <p><bold>Dark Comets in the Solar Syst</bold><bold>em</bold></p>
        <p>Since the discovery of ʻOumuamua, astronomers have identified a population of “dark comets”—SBs that exhibit measurable NGA but lack visible comae or dust tails. A notable example is 1998 KY<sub>26</sub>. It is a nearly spherical asteroid, approximately 11 meters in diameter, and is a fast rotator, having a rotational period of only 5.35 minutes. It was first observed on 2 June 1998. In 2023, 1998 KY<sub>26</sub> was identified as a possible dark comet.</p>
        <p>Dark comets are asteroids that exhibit comet-like acceleration, but visually appear as asteroids, with no coma or tail. Astronomers who study them believe the acceleration is caused by outgassing on the sunlit side. These SBs suggest that:</p>
        <p>Low-level volatile release can occur without dust entrainmentOutgassing may be spectrally or photometrically undetectableNon-gravitational forces may be more common than previously recognized</p>
        <p>Thus, ʻOumuamua may represent an extreme case within a broader, previously unrecognized population.</p>
        <p><bold>Contrast with Classical Cometary Behavi</bold><bold>or</bold></p>
        <p>The comet C/2019 Q4 (Borisov) provides a key comparison. Unlike ʻOumuamua, Borisov displayed classical cometary activity, including a prominent coma and dust tail driven by sublimation of volatiles such as H<sub>2</sub>O and CO. Its NGA is well explained by the rocket effect, in which anisotropic outgassing produces a recoil force on the nucleus. Observations further indicate a high abundance of carbon monoxide, allowing activity to persist at large heliocentric distances.</p>
      </sec>
      <sec id="sec4dot2">
        <title>4.2. Low-Albedo Asteroids</title>
        <p>The albedo in visible light ranges from about 0.9 to 0.95 for fresh snow to about 0.04 for charcoal, one of the darkest substances. A key physical property linking these SBs is their extremely low albedo. Typical values for dark bodies are 0.02 - 0.08, significantly lower than those of the Moon (~0.12) or Earth (~0.30). So, these asteroids are darker than charcoal!</p>
        <p>Main types of dark asteroids:</p>
        <p>C-type (carbonaceous): Most common (~75% of known asteroids). Rich in carbon and hydrated minerals. Very primitive (early SS material). Examples: 253 Mathilde, albedo ~0.044.D-type: Even darker and more organic-rich. Found in outer SS regions. Examples: 624 Hektor, albedo 0.025; 911 Agamemnon, albedo 0.037.P-type: low-reflectivity mixtures of carbon, silicates, and organics.</p>
        <p>Their darkness is attributed to carbon-rich composition, complex organic residues, and long-term radiation processing.</p>
        <p><bold>Connection to</bold><bold>Interstellar Objec</bold><bold>ts</bold></p>
        <p>1I/ʻOumuamua (albedo 0.04 - 0.08).2I/Borisov (albedo 0.03 - 0.04).3I/ATLAS (albedo 0.02 - 0.06).</p>
        <p>These objects are almost certainly very dark, but their exact albedo remains unconstrained. Such a low albedo implies either primitive composition (a carbon-rich, organic-coated surface) or surface processing (cosmic rays, UV, gamma radiation) over long timescales.</p>
        <p><bold>Observational Bi</bold><bold>as</bold></p>
        <p>Low-albedo bodies are difficult to detect due to their weak reflectivity and are often identified through infrared observations or deep sky surveys such as PanSTARRS. This introduces a strong observational bias, implying that many such SBs likely remain undetected.</p>
        <p><bold>Synthes</bold><bold>is</bold></p>
        <p>The combined evidence supports a unified interpretation in which:</p>
        <p>Dark comets represent a transitional population between asteroids and cometsLow albedo reflects primitive composition and/or radiation processingNGA arises from dust-poor or dust-free outgassing</p>
        <p>Within this framework, SBs such as ʻOumuamua, C/2019 Q4 (Borisov), and C/2025 N1 (ATLAS) can be understood as members of a continuous population shaped by common physical processes.</p>
      </sec>
      <sec id="sec4dot3">
        <title>4.3. ‘Oumuamua</title>
        <p>There is no detailed, high-resolution photograph of ‘Oumuamua. Because the ‘Oumuamua was so small and moving so fast, it appeared only as a single, faint point of light, even to our most powerful telescopes. The iconic “cigar-shaped” or “pancake-shaped” images seen in the media are artist’s impressions based on mathematical models of how the object’s brightness changed as it tumbled.</p>
        <p>‘Oumuamua was discovered about 40 days after it passed closest to the Sun. Major telescopes like Hubble could not be pointed at it until ‘Oumuamua was already hundreds of millions of kilometers away and fading.</p>
        <p>Because ‘Oumuamua moved faster than gravity alone could explain, scientists have proposed several theories for this NGA. Since no visible comet tail was detected, the cause remains a subject of intense debate. There were proposed different mechanisms for NGA:</p>
        <p>1) Hydrogen Outgassing (Leading Natural Theory)</p>
        <p>2) Nitrogen Iceberg</p>
        <p>3) Solar Radiation Pressure. </p>
        <p>This theory suggests the acceleration was caused simply by the physical “push” of sunlight (photons) hitting the object’s surface. The Requirement: For light alone to push ‘Oumuamua this much, the object would have to be extremely thin—less than a millimeter thick—acting like a massive sail.</p>
        <p><bold>Implication:</bold>This led to the controversial suggestion that ‘Oumuamua could be of artificial origin, such as a piece of advanced space debris or a probe. This suggestion was proposed based on eccentricity <italic>e</italic> = 1.2 of its outbound trajectory after full NGA during inbound trajectory. The first quantified value of ‘Oumuamua NGA was obtained by Micheli <italic>et al</italic>. [<xref ref-type="bibr" rid="B3">3</xref>]:</p>
        <disp-formula id="FD1">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>a</mml:mi>
                <mml:mrow>
                  <mml:mtext>NG</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>≈</mml:mo>
              <mml:mrow>
                <mml:mo>(</mml:mo>
                <mml:mrow>
                  <mml:mn>4.9</mml:mn>
                  <mml:mo>±</mml:mo>
                  <mml:mn>0.2</mml:mn>
                </mml:mrow>
                <mml:mo>)</mml:mo>
              </mml:mrow>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>6</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>m</mml:mtext>
              <mml:mo>⋅</mml:mo>
              <mml:msup>
                <mml:mtext>s</mml:mtext>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>2</mml:mn>
                </mml:mrow>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>that exceeds the NGA values for the classical comets by more than fifty times (see Section 4.6), despite the absence of a detectable dust coma, demonstrating that significant recoil forces can arise from dust-poor or dust-free outgassing.</p>
      </sec>
      <sec id="sec4dot4">
        <title>4.4. C/2019 Q4 (Borisov)</title>
        <p>Unlike ‘Oumuamua, where the acceleration was a mystery due to a lack of visible activity, C/2019 Q4 (Borisov) behaved like a “textbook” comet. Its NGA was clearly linked to the visible outgassing of gas and dust as it approached the Sun.</p>
        <p>As Borisov got closer to the Sun, its ices (specifically water and carbon monoxide) sublimated directly into gas. This gas, along with dust particles, was ejected from the nucleus in “jets”. These jets created a recoil force that pushed the comet slightly off its purely gravitational path.</p>
        <p>Observations showed that Borisov was exceptionally rich in carbon monoxide (CO), which sublimates at much lower temperatures than water ice. This allowed it to remain active and continue accelerating even at great distances from the Sun.</p>
        <p>Borisov was so “normal” that it helped astronomers understand what a typical interstellar comet looks like. Its acceleration allowed researchers to estimate its mass and density more accurately than they could for ‘Oumuamua. The mechanism of its NGA <inline-formula><mml:math display="inline"><mml:mrow><mml:msub><mml:mi> a </mml:mi><mml:mrow><mml:mtext> NG </mml:mtext></mml:mrow></mml:msub><mml:mo> ~ </mml:mo><mml:msup><mml:mrow><mml:mn> 10 </mml:mn></mml:mrow><mml:mrow><mml:mo> − </mml:mo><mml:mn> 6 </mml:mn></mml:mrow></mml:msup><mml:mtext>   </mml:mtext><mml:mtext> m </mml:mtext><mml:mo> ⋅ </mml:mo><mml:msup><mml:mtext> s </mml:mtext><mml:mrow><mml:mo> − </mml:mo><mml:mn> 2 </mml:mn></mml:mrow></mml:msup></mml:mrow></mml:math></inline-formula> (this value is much larger than the values for outgassing mechanism, see Section 4.6) remains open.</p>
      </sec>
      <sec id="sec4dot5">
        <title>4.5. C/2025 N1 (ATLAS)</title>
        <p>Recent high-precision orbit determinations of C/2025 N1 (ATLAS) provide strong evidence for significant NGA well above the levels typically observed in long-period comets. Eubanks <italic>et al</italic>. incorporated six additional observations obtained from two interplanetary spacecraft into the orbital solution. These measurements, acquired from vantage points and epochs inaccessible to ground-based observatories, reduced the formal uncertainties in the derived NGA parameters by approximately 20% - 40% compared to solutions based solely on ground-based data collected between May and December 2025 [<xref ref-type="bibr" rid="B4">4</xref>].</p>
        <p>Using this expanded dataset, they determined an NGA vector (scaled to 1 AU) of:</p>
        <disp-formula id="FD2">
          <mml:math>
            <mml:mrow>
              <mml:mrow>
                <mml:mo>(</mml:mo>
                <mml:mrow>
                  <mml:mn>89.3</mml:mn>
                  <mml:mo>±</mml:mo>
                  <mml:mn>4.6</mml:mn>
                </mml:mrow>
                <mml:mo>)</mml:mo>
              </mml:mrow>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>9</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>au</mml:mtext>
              <mml:mo>⋅</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mtext>day</mml:mtext>
                </mml:mrow>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>2</mml:mn>
                </mml:mrow>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>which corresponds to:</p>
        <disp-formula id="FD3">
          <mml:math>
            <mml:mrow>
              <mml:mrow>
                <mml:mo>(</mml:mo>
                <mml:mrow>
                  <mml:mn>1.79</mml:mn>
                  <mml:mo>±</mml:mo>
                  <mml:mn>0.09</mml:mn>
                </mml:mrow>
                <mml:mo>)</mml:mo>
              </mml:mrow>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>6</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>m</mml:mtext>
              <mml:mo>⋅</mml:mo>
              <mml:msup>
                <mml:mtext>s</mml:mtext>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>2</mml:mn>
                </mml:mrow>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>Independent analyses by several authors yield comparable or even larger values, as summarized in <bold>Table 2</bold>.</p>
        <p>According to <italic>Jet Propulsion Laboratory</italic>: <italic>Small</italic>-<italic>Body Database Lookup</italic>, the latest values of NGA for so named “interstellar comets” are presented in <bold>Table 3</bold>.</p>
        <p><bold>Table 2.</bold> Reported non-gravitational accelerations of C/2025 N1 (ATLAS).</p>
        <table-wrap id="tbl3">
          <label>Table 3</label>
          <table>
            <tbody>
              <tr>
                <td>
                  <bold>##</bold>
                </td>
                <td>
                  <bold>Authors</bold>
                </td>
                <td>
                  <bold>NGA (m</bold>
                  <bold>∙</bold>
                  <bold>s</bold>
                  <bold>
                    <sup>−2</sup>
                  </bold>
                  <bold>)</bold>
                </td>
                <td>
                  <bold>Reference</bold>
                </td>
              </tr>
              <tr>
                <td>1</td>
                <td>
                  Eubanks,
                  <italic>et al</italic>
                  .
                </td>
                <td>
                  <inline-formula>
                    <mml:math>
                      <mml:mrow>
                        <mml:mrow>
                          <mml:mo>(</mml:mo>
                          <mml:mrow>
                            <mml:mn>1.79</mml:mn>
                            <mml:mo>±</mml:mo>
                            <mml:mn>0.09</mml:mn>
                          </mml:mrow>
                          <mml:mo>)</mml:mo>
                        </mml:mrow>
                        <mml:mo>×</mml:mo>
                        <mml:msup>
                          <mml:mrow>
                            <mml:mn>10</mml:mn>
                          </mml:mrow>
                          <mml:mrow>
                            <mml:mo>−</mml:mo>
                            <mml:mn>6</mml:mn>
                          </mml:mrow>
                        </mml:msup>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
                <td>
                  [
                  <xref ref-type="bibr" rid="B4">4</xref>
                  ]
                </td>
              </tr>
              <tr>
                <td>2</td>
                <td>Neukart</td>
                <td>
                  <inline-formula>
                    <mml:math>
                      <mml:mrow>
                        <mml:mrow>
                          <mml:mo>(</mml:mo>
                          <mml:mrow>
                            <mml:mn>3.0</mml:mn>
                            <mml:mo>±</mml:mo>
                            <mml:mn>0.8</mml:mn>
                          </mml:mrow>
                          <mml:mo>)</mml:mo>
                        </mml:mrow>
                        <mml:mo>×</mml:mo>
                        <mml:msup>
                          <mml:mrow>
                            <mml:mn>10</mml:mn>
                          </mml:mrow>
                          <mml:mrow>
                            <mml:mo>−</mml:mo>
                            <mml:mn>5</mml:mn>
                          </mml:mrow>
                        </mml:msup>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
                <td>
                  [
                  <xref ref-type="bibr" rid="B5">5</xref>
                  ]
                </td>
              </tr>
              <tr>
                <td>3</td>
                <td>Scarmato</td>
                <td>
                  <inline-formula>
                    <mml:math display="inline">
                      <mml:mrow>
                        <mml:mo>~</mml:mo>
                        <mml:mn>0.5</mml:mn>
                        <mml:mo>×</mml:mo>
                        <mml:msup>
                          <mml:mrow>
                            <mml:mn>10</mml:mn>
                          </mml:mrow>
                          <mml:mrow>
                            <mml:mo>−</mml:mo>
                            <mml:mn>6</mml:mn>
                          </mml:mrow>
                        </mml:msup>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
                <td>
                  [
                  <xref ref-type="bibr" rid="B6">6</xref>
                  ]
                </td>
              </tr>
              <tr>
                <td>4</td>
                <td>Ahuja and Ganesh</td>
                <td>
                  <inline-formula>
                    <mml:math>
                      <mml:mrow>
                        <mml:mo>~</mml:mo>
                        <mml:msup>
                          <mml:mrow>
                            <mml:mn>10</mml:mn>
                          </mml:mrow>
                          <mml:mrow>
                            <mml:mo>−</mml:mo>
                            <mml:mn>6</mml:mn>
                          </mml:mrow>
                        </mml:msup>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
                <td>
                  [
                  <xref ref-type="bibr" rid="B7">7</xref>
                  ]
                </td>
              </tr>
              <tr>
                <td>5</td>
                <td>Spada, Królikowska, and Dones</td>
                <td>
                  <inline-formula>
                    <mml:math>
                      <mml:mrow>
                        <mml:mrow>
                          <mml:mo>(</mml:mo>
                          <mml:mrow>
                            <mml:mn>1.13</mml:mn>
                            <mml:mo>±</mml:mo>
                            <mml:mn>0.036</mml:mn>
                          </mml:mrow>
                          <mml:mo>)</mml:mo>
                        </mml:mrow>
                        <mml:mo>×</mml:mo>
                        <mml:msup>
                          <mml:mrow>
                            <mml:mn>10</mml:mn>
                          </mml:mrow>
                          <mml:mrow>
                            <mml:mo>−</mml:mo>
                            <mml:mn>6</mml:mn>
                          </mml:mrow>
                        </mml:msup>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
                <td>
                  [
                  <xref ref-type="bibr" rid="B8">8</xref>
                  ]
                </td>
              </tr>
            </tbody>
          </table>
        </table-wrap>
        <p><bold>Table 3.</bold> Latest non-gravitational accelerations of “interstellar objects”.</p>
        <table-wrap id="tbl4">
          <label>Table 4</label>
          <table>
            <tbody>
              <tr>
                <td>
                  <bold>##</bold>
                </td>
                <td>
                  <bold>Small Objects</bold>
                </td>
                <td>
                  <bold>NGA (m</bold>
                  <bold>∙</bold>
                  <bold>s</bold>
                  <bold>
                    <sup>−2</sup>
                  </bold>
                  <bold>)</bold>
                </td>
                <td>
                  <bold>Reference</bold>
                </td>
              </tr>
              <tr>
                <td>1</td>
                <td>1I/ʻOumuamua</td>
                <td>
                  <inline-formula>
                    <mml:math>
                      <mml:mrow>
                        <mml:mrow>
                          <mml:mo>(</mml:mo>
                          <mml:mrow>
                            <mml:mn>5.6</mml:mn>
                            <mml:mo>±</mml:mo>
                            <mml:mn>0.72</mml:mn>
                          </mml:mrow>
                          <mml:mo>)</mml:mo>
                        </mml:mrow>
                        <mml:mo>×</mml:mo>
                        <mml:msup>
                          <mml:mrow>
                            <mml:mn>10</mml:mn>
                          </mml:mrow>
                          <mml:mrow>
                            <mml:mo>−</mml:mo>
                            <mml:mn>6</mml:mn>
                          </mml:mrow>
                        </mml:msup>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
                <td>
                  [
                  <xref ref-type="bibr" rid="B9">9</xref>
                  ]
                </td>
              </tr>
              <tr>
                <td>2</td>
                <td>2I/Borisov</td>
                <td>
                  <inline-formula>
                    <mml:math>
                      <mml:mrow>
                        <mml:mrow>
                          <mml:mo>(</mml:mo>
                          <mml:mrow>
                            <mml:mn>0.98</mml:mn>
                            <mml:mo>±</mml:mo>
                            <mml:mn>0.08</mml:mn>
                          </mml:mrow>
                          <mml:mo>)</mml:mo>
                        </mml:mrow>
                        <mml:mo>×</mml:mo>
                        <mml:msup>
                          <mml:mrow>
                            <mml:mn>10</mml:mn>
                          </mml:mrow>
                          <mml:mrow>
                            <mml:mo>−</mml:mo>
                            <mml:mn>6</mml:mn>
                          </mml:mrow>
                        </mml:msup>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
                <td>
                  [
                  <xref ref-type="bibr" rid="B10">10</xref>
                  ]
                </td>
              </tr>
              <tr>
                <td>3</td>
                <td>3I/ATLAS</td>
                <td>
                  <inline-formula>
                    <mml:math>
                      <mml:mrow>
                        <mml:mrow>
                          <mml:mo>(</mml:mo>
                          <mml:mrow>
                            <mml:mn>1.06</mml:mn>
                            <mml:mo>±</mml:mo>
                            <mml:mn>0.024</mml:mn>
                          </mml:mrow>
                          <mml:mo>)</mml:mo>
                        </mml:mrow>
                        <mml:mo>×</mml:mo>
                        <mml:msup>
                          <mml:mrow>
                            <mml:mn>10</mml:mn>
                          </mml:mrow>
                          <mml:mrow>
                            <mml:mo>−</mml:mo>
                            <mml:mn>6</mml:mn>
                          </mml:mrow>
                        </mml:msup>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
                <td>
                  [
                  <xref ref-type="bibr" rid="B11">11</xref>
                  ]
                </td>
              </tr>
            </tbody>
          </table>
        </table-wrap>
        <p>A key result emerging from these studies is that the characteristic magnitude of NGA satisfies:</p>
        <disp-formula id="FD4">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>a</mml:mi>
                <mml:mrow>
                  <mml:mtext>NG</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>≳</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>6</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>m</mml:mtext>
              <mml:mo>⋅</mml:mo>
              <mml:msup>
                <mml:mtext>s</mml:mtext>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>2</mml:mn>
                </mml:mrow>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>This value is one to four orders of magnitude larger than the typical range observed in comets (Section 4.6).</p>
        <p><bold>Implicatio</bold><bold>ns</bold></p>
        <p>Such an unusually large acceleration cannot be readily explained by standard mechanisms:</p>
        <p>Outgassing: would require unrealistically high mass-loss rates or extreme anisotropyRadiation pressure: insufficient for an object of typical cometary size and massThermal effects (Yarkovsky/YORP): too weak by several orders of magnitude</p>
        <p>Therefore, <bold>C/2025 N1</bold> (ATLAS) occupies a distinct dynamical regime, in which the conventional framework of cometary physics appears insufficient.</p>
        <p>This discrepancy strongly suggests the presence of an additional or alternative acceleration mechanism. Within the present framework, such behavior is naturally interpreted as the result of an internal energy conversion, in which the rotational energy of a nucleus is partially transformed into translational kinetic energy of SB3.</p>
      </sec>
      <sec id="sec4dot6">
        <title>4.6. Sources of Non-Gravitational Accelerations</title>
        <p>NGAs are measurable deviations from purely gravitational motion, arising from internal or surface processes, as well as interactions with radiation and plasma. Although typically small in magnitude, NGAs play a crucial role in the orbital evolution of small bodies, particularly those on near-parabolic trajectories.</p>
        <p><bold>Principal</bold><bold>Sources</bold><bold>of N</bold><bold>GA</bold></p>
        <p><bold>1</bold><bold>) Outgassing</bold><bold>(dominant for comets).</bold>Asymmetric sublimation of volatile ices produces reactive forces that alter the trajectory.</p>
        <p>Typical magnitude near 1 AU:</p>
        <disp-formula id="FD5">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>a</mml:mi>
                <mml:mrow>
                  <mml:mtext>NG</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>~</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>to</mml:mtext>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>7</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>m</mml:mtext>
              <mml:mo>⋅</mml:mo>
              <mml:msup>
                <mml:mtext>s</mml:mtext>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>2</mml:mn>
                </mml:mrow>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>Effects:shifts in perihelion timing (hours to days)changes in eccentricity at the 10<sup>−7</sup> - 10<sup>−6</sup> levelmodification of inferred original orbits</p>
        <p><bold>2</bold><bold>) Yarkovsky effect</bold><bold>(thermal recoil).</bold> Anisotropic thermal emission from a rotating body produces a small thrust.</p>
        <p>Typical magnitude:</p>
        <disp-formula id="FD6">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>a</mml:mi>
                <mml:mrow>
                  <mml:mtext>Yark</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>~</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>13</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>to</mml:mtext>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>m</mml:mtext>
              <mml:mo>⋅</mml:mo>
              <mml:msup>
                <mml:mtext>s</mml:mtext>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>2</mml:mn>
                </mml:mrow>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>Important for:long-term orbital driftnear-Earth asteroid trajectory prediction</p>
        <p><bold>3</bold><bold>) YORP effect</bold><bold>(rotational dynamics).</bold> Radiation and thermal emission exert torques that modify spin rate and axis orientation.</p>
        <p>Consequences:spin-up or spin-downchanges in obliquitypossible structural disruption or fissionindirect influence on orbital evolution via altered outgassing geometry</p>
        <p><bold>4</bold><bold>) Radiation pressure.</bold>Momentum transfer from solar photons affects small or low-mass objects.</p>
        <p>Particularly relevant for:very small bodieslow-density or high area-to-mass ratio objects</p>
        <p><bold>Summa</bold><bold>ry</bold></p>
        <p>NGA in SS bodies arise primarily from outgassing, radiation pressure, and thermal effects. Their typical magnitudes (10<sup>−10</sup> - 10<sup>−7</sup> m s<sup>−2</sup>) are small but dynamically significant, especially for long-period comets near the parabolic limit, where even minute perturbations can produce large changes in inferred orbital parameters.</p>
        <p>However, these known mechanisms are insufficient to explain strongly hyperbolic trajectories such as that reported for C/2025 N1 (ATLAS). This discrepancy motivates the exploration of alternative acceleration mechanisms.</p>
      </sec>
      <sec id="sec4dot7">
        <title>4.7. Origin of Comets and Asteroids</title>
        <p>Comets and asteroids are widely understood as remnants of the early SS, formed approximately 4.6 billion years ago from the protoplanetary disk surrounding the young Sun. Their formation reflects the thermal gradient within this disk:</p>
        <p>Inner SS (high temperature): Formation of rocky and metallic bodies → asteroids.Outer SS (low temperature): Condensation of volatile ices mixed with dust → comets.</p>
        <p>Asteroids primarily formed in the region now occupied by the asteroid belt, where gravitational perturbations from Jupiter inhibited accretion into a full-sized planet. Comets formed beyond the “snow line,” where volatile compounds such as water, CO<sub>2</sub>, methane, and ammonia could condense.</p>
        <p>Subsequent gravitational interactions with the giant planets redistributed these bodies:</p>
        <p>Kuiper Belt: reservoir of short-period cometsOort Cloud: source of long-period comets</p>
        <p>This standard model implies a common origin in the protoplanetary disk, with present-day differences arising from thermal history and dynamical evolution. At the same time, growing observational evidence supports a continuum between asteroids and comets, blurring traditional classification boundaries.</p>
        <p><bold>Key question.</bold>What is the ultimate origin of the material—dust, metals, ices, and complex molecules—that formed these primordial bodies? This question remains open and is central to alternative cosmological frameworks such as WUC.</p>
      </sec>
    </sec>
    <sec id="sec5">
      <title>
        5. Multiworld Framework [
        <xref ref-type="bibr" rid="B1">1</xref>
        ]
      </title>
      <p>The concept of multiple coexisting physical regimes has been previously hinted at in the literature. As noted by Oreshko, Pyotr Kapitsa suggested that <italic>ball lightning may represent a</italic>“<italic>window</italic>”<italic>into another world</italic> [<xref ref-type="bibr" rid="B12">12</xref>]. Motivated by this idea, we developed a hierarchical Multiworld framework consisting of Macro-world, Large-world, Small-world, and Micro-world.</p>
      <p>In contrast to the standard cosmological paradigm invoking dark matter, WUC assumes that the World is composed of:</p>
      <p>Ordinary Matter (protons, electrons, photons, neutrinos)Universe-Created Matter (UCM), consisting of Universe-Created Particles (UCPs)</p>
      <p>These components interact through a hierarchy of interactions with different strengths and characteristic scales.</p>
      <sec id="sec5dot1">
        <title>5.1. Macro-World (Gravitational Regime)</title>
        <p>Gravity is described by a scale-dependent gravitational parameter:</p>
        <disp-formula id="FD7">
          <mml:math>
            <mml:mrow>
              <mml:mi>G</mml:mi>
              <mml:mo>=</mml:mo>
              <mml:msub>
                <mml:mi>G</mml:mi>
                <mml:mn>0</mml:mn>
              </mml:msub>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mi>Q</mml:mi>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>1</mml:mn>
                </mml:mrow>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>where: <inline-formula><mml:math><mml:mrow><mml:msub><mml:mi> G </mml:mi><mml:mn> 0 </mml:mn></mml:msub><mml:mo> = </mml:mo><mml:mfrac><mml:mrow><mml:msup><mml:mi> a </mml:mi><mml:mn> 2 </mml:mn></mml:msup><mml:msup><mml:mi> c </mml:mi><mml:mn> 4 </mml:mn></mml:msup></mml:mrow><mml:mrow><mml:mn> 8 </mml:mn><mml:mi> π </mml:mi><mml:mi> h </mml:mi><mml:mi> c </mml:mi></mml:mrow></mml:mfrac></mml:mrow></mml:math></inline-formula> is an extrapolated value of <inline-formula><mml:math display="inline"><mml:mi> G </mml:mi></mml:math></inline-formula> at <inline-formula><mml:math><mml:mrow><mml:mi> Q </mml:mi><mml:mo> = </mml:mo><mml:mn> 1 </mml:mn></mml:mrow></mml:math></inline-formula> , <inline-formula><mml:math display="inline"><mml:mi> h </mml:mi></mml:math></inline-formula> is the Planck constant, <inline-formula><mml:math display="inline"><mml:mi> c </mml:mi></mml:math></inline-formula> is a gravitodynamic constant, <inline-formula><mml:math><mml:mi> a </mml:mi></mml:math></inline-formula> is a basic length unit:</p>
        <disp-formula id="FD8">
          <mml:math>
            <mml:mrow>
              <mml:mi>a</mml:mi>
              <mml:mo>=</mml:mo>
              <mml:mn>1.7705641</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>14</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>m</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p><inline-formula><mml:math display="inline"><mml:mi> Q </mml:mi></mml:math></inline-formula> in the present Epoch equals <inline-formula><mml:math><mml:mrow><mml:mi> Q </mml:mi><mml:mo> = </mml:mo><mml:mn> 0.759972 </mml:mn><mml:mo> × </mml:mo><mml:msup><mml:mrow><mml:mn> 10 </mml:mn></mml:mrow><mml:mrow><mml:mn> 40 </mml:mn></mml:mrow></mml:msup></mml:mrow></mml:math></inline-formula> . The corresponding characteristic scale (radius of the World <inline-formula><mml:math display="inline"><mml:mi> R </mml:mi></mml:math></inline-formula> ) is:</p>
        <disp-formula id="FD9">
          <mml:math>
            <mml:mrow>
              <mml:mi>R</mml:mi>
              <mml:mo>=</mml:mo>
              <mml:mi>a</mml:mi>
              <mml:mo>×</mml:mo>
              <mml:mi>Q</mml:mi>
              <mml:mo>=</mml:mo>
              <mml:mn>1.34558</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mn>26</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>m</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>The total mass and average critical density of the Macro-world are:</p>
        <disp-formula id="FD10">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>M</mml:mi>
                <mml:mrow>
                  <mml:mtext>MW</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mn>6</mml:mn>
              <mml:msup>
                <mml:mi>π</mml:mi>
                <mml:mn>2</mml:mn>
              </mml:msup>
              <mml:msub>
                <mml:mi>m</mml:mi>
                <mml:mn>0</mml:mn>
              </mml:msub>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mi>Q</mml:mi>
                <mml:mn>2</mml:mn>
              </mml:msup>
              <mml:mo>=</mml:mo>
              <mml:mn>4.27</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mn>53</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>kg</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <disp-formula id="FD11">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>ρ</mml:mi>
                <mml:mrow>
                  <mml:mtext>MW</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mn>3</mml:mn>
              <mml:msub>
                <mml:mi>ρ</mml:mi>
                <mml:mn>0</mml:mn>
              </mml:msub>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mi>Q</mml:mi>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>1</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mo>=</mml:mo>
              <mml:mn>8.88</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>27</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>kg</mml:mtext>
              <mml:mo>⋅</mml:mo>
              <mml:msup>
                <mml:mtext>m</mml:mtext>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>3</mml:mn>
                </mml:mrow>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>where <inline-formula><mml:math><mml:mrow><mml:msub><mml:mi> m </mml:mi><mml:mn> 0 </mml:mn></mml:msub></mml:mrow></mml:math></inline-formula> is a basic mass unit: <inline-formula><mml:math><mml:mrow><mml:msub><mml:mi> m </mml:mi><mml:mn> 0 </mml:mn></mml:msub><mml:mo> = </mml:mo><mml:mrow><mml:mi> h </mml:mi><mml:mo> / </mml:mo><mml:mrow><mml:mi> a </mml:mi><mml:mi> c </mml:mi></mml:mrow></mml:mrow></mml:mrow></mml:math></inline-formula> and <inline-formula><mml:math><mml:mrow><mml:msub><mml:mi> ρ </mml:mi><mml:mn> 0 </mml:mn></mml:msub></mml:mrow></mml:math></inline-formula> is a basic density unit:</p>
        <disp-formula id="FD12">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>ρ</mml:mi>
                <mml:mn>0</mml:mn>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mrow>
                <mml:mi>h</mml:mi>
                <mml:mo>/</mml:mo>
                <mml:mrow>
                  <mml:mi>c</mml:mi>
                  <mml:msup>
                    <mml:mi>a</mml:mi>
                    <mml:mn>4</mml:mn>
                  </mml:msup>
                </mml:mrow>
              </mml:mrow>
            </mml:mrow>
          </mml:math>
        </disp-formula>
      </sec>
      <sec id="sec5dot2">
        <title>5.2. Hierarchy of Interactions</title>
        <p>WUC introduces three additional interactions beyond gravity: Weak, Super-Weak, and Extremely-Weak, characterized by the following parameters respectively:</p>
        <disp-formula id="FD13">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>G</mml:mi>
                <mml:mtext>W</mml:mtext>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:msub>
                <mml:mi>G</mml:mi>
                <mml:mi>O</mml:mi>
              </mml:msub>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mi>Q</mml:mi>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mrow>
                    <mml:mn>1</mml:mn>
                    <mml:mo>/</mml:mo>
                    <mml:mn>4</mml:mn>
                  </mml:mrow>
                </mml:mrow>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <disp-formula id="FD14">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>G</mml:mi>
                <mml:mrow>
                  <mml:mtext>SW</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:msub>
                <mml:mi>G</mml:mi>
                <mml:mi>O</mml:mi>
              </mml:msub>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mi>Q</mml:mi>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mrow>
                    <mml:mn>1</mml:mn>
                    <mml:mo>/</mml:mo>
                    <mml:mn>2</mml:mn>
                  </mml:mrow>
                </mml:mrow>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <disp-formula id="FD15">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>G</mml:mi>
                <mml:mrow>
                  <mml:mtext>EW</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:msub>
                <mml:mi>G</mml:mi>
                <mml:mi>O</mml:mi>
              </mml:msub>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mi>Q</mml:mi>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mrow>
                    <mml:mn>3</mml:mn>
                    <mml:mo>/</mml:mo>
                    <mml:mn>4</mml:mn>
                  </mml:mrow>
                </mml:mrow>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>Each interaction defines the integrity and scale of the corresponding world (<bold>Table 4</bold>).</p>
        <p><bold>Table 4.</bold> Parameters of the Multiworld.</p>
        <table-wrap id="tbl5">
          <label>Table 5</label>
          <table>
            <tbody>
              <tr>
                <td>
                  <bold>Type of</bold>
                  <bold>World</bold>
                </td>
                <td>
                  <bold>Type of</bold>
                  <bold>Interaction</bold>
                </td>
                <td>
                  <bold>Rel. Interaction</bold>
                  <bold>Parameter,</bold>
                  <inline-formula>
                    <mml:math>
                      <mml:mrow>
                        <mml:mrow>
                          <mml:mi>G</mml:mi>
                          <mml:mo>/</mml:mo>
                          <mml:mrow>
                            <mml:msub>
                              <mml:mi>G</mml:mi>
                              <mml:mn>0</mml:mn>
                            </mml:msub>
                          </mml:mrow>
                        </mml:mrow>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
                <td>
                  <bold>Rel. Range of Interact,</bold>
                  <inline-formula>
                    <mml:math>
                      <mml:mrow>
                        <mml:mrow>
                          <mml:mrow>
                            <mml:msub>
                              <mml:mi>R</mml:mi>
                              <mml:mrow>
                                <mml:mi>m</mml:mi>
                                <mml:mi>a</mml:mi>
                                <mml:mi>x</mml:mi>
                              </mml:mrow>
                            </mml:msub>
                          </mml:mrow>
                          <mml:mo>/</mml:mo>
                          <mml:mi>a</mml:mi>
                        </mml:mrow>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
                <td>
                  <bold>Rel. Mass,</bold>
                  <inline-formula>
                    <mml:math display="inline">
                      <mml:mrow>
                        <mml:mrow>
                          <mml:mrow>
                            <mml:msub>
                              <mml:mi>M</mml:mi>
                              <mml:mrow>
                                <mml:mi>m</mml:mi>
                                <mml:mi>a</mml:mi>
                                <mml:mi>x</mml:mi>
                              </mml:mrow>
                            </mml:msub>
                          </mml:mrow>
                          <mml:mo>/</mml:mo>
                          <mml:mrow>
                            <mml:mn>4</mml:mn>
                            <mml:mi>π</mml:mi>
                            <mml:msub>
                              <mml:mi>m</mml:mi>
                              <mml:mn>0</mml:mn>
                            </mml:msub>
                          </mml:mrow>
                        </mml:mrow>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
                <td>
                  <bold>Rel. Density,</bold>
                  <inline-formula>
                    <mml:math display="inline">
                      <mml:mrow>
                        <mml:mrow>
                          <mml:mi>ρ</mml:mi>
                          <mml:mo>/</mml:mo>
                          <mml:mrow>
                            <mml:mn>3</mml:mn>
                            <mml:msub>
                              <mml:mi>ρ</mml:mi>
                              <mml:mn>0</mml:mn>
                            </mml:msub>
                          </mml:mrow>
                        </mml:mrow>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
              </tr>
              <tr>
                <td>Macro-World</td>
                <td>Gravity</td>
                <td>
                  <inline-formula>
                    <mml:math>
                      <mml:mrow>
                        <mml:msup>
                          <mml:mi>Q</mml:mi>
                          <mml:mrow>
                            <mml:mo>−</mml:mo>
                            <mml:mn>1</mml:mn>
                          </mml:mrow>
                        </mml:msup>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
                <td>
                  <inline-formula>
                    <mml:math>
                      <mml:mi>Q</mml:mi>
                    </mml:math>
                  </inline-formula>
                </td>
                <td>
                  <inline-formula>
                    <mml:math>
                      <mml:mrow>
                        <mml:mn>1.5</mml:mn>
                        <mml:mi>π</mml:mi>
                        <mml:mo>×</mml:mo>
                        <mml:msup>
                          <mml:mi>Q</mml:mi>
                          <mml:mn>2</mml:mn>
                        </mml:msup>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
                <td>
                  <inline-formula>
                    <mml:math>
                      <mml:mrow>
                        <mml:msup>
                          <mml:mi>Q</mml:mi>
                          <mml:mrow>
                            <mml:mo>−</mml:mo>
                            <mml:mn>1</mml:mn>
                          </mml:mrow>
                        </mml:msup>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
              </tr>
              <tr>
                <td>Large-World</td>
                <td>Extremely-Weak</td>
                <td>
                  <inline-formula>
                    <mml:math>
                      <mml:mrow>
                        <mml:msup>
                          <mml:mi>Q</mml:mi>
                          <mml:mrow>
                            <mml:mo>−</mml:mo>
                            <mml:mrow>
                              <mml:mn>3</mml:mn>
                              <mml:mo>/</mml:mo>
                              <mml:mn>4</mml:mn>
                            </mml:mrow>
                          </mml:mrow>
                        </mml:msup>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
                <td>
                  <inline-formula>
                    <mml:math display="inline">
                      <mml:mrow>
                        <mml:msup>
                          <mml:mi>Q</mml:mi>
                          <mml:mrow>
                            <mml:mrow>
                              <mml:mn>3</mml:mn>
                              <mml:mo>/</mml:mo>
                              <mml:mn>4</mml:mn>
                            </mml:mrow>
                          </mml:mrow>
                        </mml:msup>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
                <td>
                  <inline-formula>
                    <mml:math display="inline">
                      <mml:mrow>
                        <mml:msup>
                          <mml:mi>Q</mml:mi>
                          <mml:mrow>
                            <mml:mrow>
                              <mml:mn>3</mml:mn>
                              <mml:mo>/</mml:mo>
                              <mml:mn>2</mml:mn>
                            </mml:mrow>
                          </mml:mrow>
                        </mml:msup>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
                <td>
                  <inline-formula>
                    <mml:math>
                      <mml:mrow>
                        <mml:msup>
                          <mml:mi>Q</mml:mi>
                          <mml:mrow>
                            <mml:mo>−</mml:mo>
                            <mml:mrow>
                              <mml:mn>3</mml:mn>
                              <mml:mo>/</mml:mo>
                              <mml:mn>4</mml:mn>
                            </mml:mrow>
                          </mml:mrow>
                        </mml:msup>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
              </tr>
              <tr>
                <td>Small-World</td>
                <td>Super-Weak</td>
                <td>
                  <inline-formula>
                    <mml:math display="inline">
                      <mml:mrow>
                        <mml:msup>
                          <mml:mi>Q</mml:mi>
                          <mml:mrow>
                            <mml:mo>−</mml:mo>
                            <mml:mrow>
                              <mml:mn>1</mml:mn>
                              <mml:mo>/</mml:mo>
                              <mml:mn>2</mml:mn>
                            </mml:mrow>
                          </mml:mrow>
                        </mml:msup>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
                <td>
                  <inline-formula>
                    <mml:math display="inline">
                      <mml:mrow>
                        <mml:msup>
                          <mml:mi>Q</mml:mi>
                          <mml:mrow>
                            <mml:mrow>
                              <mml:mn>1</mml:mn>
                              <mml:mo>/</mml:mo>
                              <mml:mn>2</mml:mn>
                            </mml:mrow>
                          </mml:mrow>
                        </mml:msup>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
                <td>
                  <inline-formula>
                    <mml:math>
                      <mml:mi>Q</mml:mi>
                    </mml:math>
                  </inline-formula>
                </td>
                <td>
                  <inline-formula>
                    <mml:math display="inline">
                      <mml:mrow>
                        <mml:msup>
                          <mml:mi>Q</mml:mi>
                          <mml:mrow>
                            <mml:mo>−</mml:mo>
                            <mml:mrow>
                              <mml:mn>1</mml:mn>
                              <mml:mo>/</mml:mo>
                              <mml:mn>2</mml:mn>
                            </mml:mrow>
                          </mml:mrow>
                        </mml:msup>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
              </tr>
              <tr>
                <td>Micro-World</td>
                <td>Weak</td>
                <td>
                  <inline-formula>
                    <mml:math display="inline">
                      <mml:mrow>
                        <mml:msup>
                          <mml:mi>Q</mml:mi>
                          <mml:mrow>
                            <mml:mo>−</mml:mo>
                            <mml:mrow>
                              <mml:mn>1</mml:mn>
                              <mml:mo>/</mml:mo>
                              <mml:mn>4</mml:mn>
                            </mml:mrow>
                          </mml:mrow>
                        </mml:msup>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
                <td>
                  <inline-formula>
                    <mml:math display="inline">
                      <mml:mrow>
                        <mml:msup>
                          <mml:mi>Q</mml:mi>
                          <mml:mrow>
                            <mml:mrow>
                              <mml:mn>1</mml:mn>
                              <mml:mo>/</mml:mo>
                              <mml:mn>4</mml:mn>
                            </mml:mrow>
                          </mml:mrow>
                        </mml:msup>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
                <td>
                  <inline-formula>
                    <mml:math display="inline">
                      <mml:mrow>
                        <mml:msup>
                          <mml:mi>Q</mml:mi>
                          <mml:mrow>
                            <mml:mrow>
                              <mml:mn>1</mml:mn>
                              <mml:mo>/</mml:mo>
                              <mml:mn>2</mml:mn>
                            </mml:mrow>
                          </mml:mrow>
                        </mml:msup>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
                <td>
                  <inline-formula>
                    <mml:math display="inline">
                      <mml:mrow>
                        <mml:msup>
                          <mml:mi>Q</mml:mi>
                          <mml:mrow>
                            <mml:mo>−</mml:mo>
                            <mml:mrow>
                              <mml:mn>1</mml:mn>
                              <mml:mo>/</mml:mo>
                              <mml:mn>4</mml:mn>
                            </mml:mrow>
                          </mml:mrow>
                        </mml:msup>
                      </mml:mrow>
                    </mml:math>
                  </inline-formula>
                </td>
              </tr>
            </tbody>
          </table>
        </table-wrap>
      </sec>
      <sec id="sec5dot3">
        <title>5.3. Large-World (Extremely-Weak Interaction)</title>
        <p>The Large-world is governed by the extremely-weak interaction, approximately 10 orders of magnitude stronger than gravity. Its characteristic range is:</p>
        <disp-formula id="FD16">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>R</mml:mi>
                <mml:mrow>
                  <mml:mtext>EW</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mi>a</mml:mi>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mi>Q</mml:mi>
                <mml:mrow>
                  <mml:mrow>
                    <mml:mn>3</mml:mn>
                    <mml:mo>/</mml:mo>
                    <mml:mn>4</mml:mn>
                  </mml:mrow>
                </mml:mrow>
              </mml:msup>
              <mml:mo>=</mml:mo>
              <mml:mn>1.44</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mn>16</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>m</mml:mtext>
              <mml:mo>≈</mml:mo>
              <mml:mn>1.52</mml:mn>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>ly</mml:mtext>
              <mml:mo>≈</mml:mo>
              <mml:mn>96335</mml:mn>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>AU</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>This scale defines the boundary of Extra-Solar Systems (ESS), interpreted as spherical structures separating Solar-type systems from the Interstellar Medium.</p>
        <p>The maximum total mass of such a system is:</p>
        <disp-formula id="FD17">
          <mml:math display="inline">
            <mml:mrow>
              <mml:msub>
                <mml:mi>M</mml:mi>
                <mml:mrow>
                  <mml:mtext>ESS</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mn>4</mml:mn>
              <mml:mi>π</mml:mi>
              <mml:msub>
                <mml:mi>m</mml:mi>
                <mml:mn>0</mml:mn>
              </mml:msub>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mi>Q</mml:mi>
                <mml:mrow>
                  <mml:mrow>
                    <mml:mn>3</mml:mn>
                    <mml:mo>/</mml:mo>
                    <mml:mn>2</mml:mn>
                  </mml:mrow>
                </mml:mrow>
              </mml:msup>
              <mml:mo>=</mml:mo>
              <mml:mn>1.04</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mn>33</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>kg</mml:mtext>
              <mml:mo>≈</mml:mo>
              <mml:mn>523</mml:mn>
              <mml:msub>
                <mml:mi>M</mml:mi>
                <mml:mo>⊙</mml:mo>
              </mml:msub>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>with a corresponding maximum stellar mass:</p>
        <disp-formula id="FD18">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>M</mml:mi>
                <mml:mrow>
                  <mml:mtext>Star</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mrow>
                <mml:mn>1</mml:mn>
                <mml:mo>/</mml:mo>
                <mml:mn>3</mml:mn>
              </mml:mrow>
              <mml:msub>
                <mml:mi>M</mml:mi>
                <mml:mrow>
                  <mml:mtext>ESS</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>≈</mml:mo>
              <mml:mn>174</mml:mn>
              <mml:msub>
                <mml:mi>M</mml:mi>
                <mml:mo>⊙</mml:mo>
              </mml:msub>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>The average density:</p>
        <disp-formula id="FD19">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>ρ</mml:mi>
                <mml:mrow>
                  <mml:mtext>EW</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mn>3</mml:mn>
              <mml:msub>
                <mml:mi>ρ</mml:mi>
                <mml:mn>0</mml:mn>
              </mml:msub>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mi>Q</mml:mi>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mrow>
                    <mml:mn>3</mml:mn>
                    <mml:mo>/</mml:mo>
                    <mml:mn>4</mml:mn>
                  </mml:mrow>
                </mml:mrow>
              </mml:msup>
              <mml:mo>=</mml:mo>
              <mml:mn>8.29</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>17</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>kg</mml:mtext>
              <mml:mo>⋅</mml:mo>
              <mml:msup>
                <mml:mtext>m</mml:mtext>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>3</mml:mn>
                </mml:mrow>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>exceeds the critical density by ten orders of magnitude.</p>
      </sec>
      <sec id="sec5dot4">
        <title>5.4. Small-World (Super-Weak Interaction)</title>
        <p>The Small-world is governed by the super-weak interaction, approximately 20 orders of magnitude stronger than gravity. Its characteristic range is:</p>
        <disp-formula id="FD20">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>R</mml:mi>
                <mml:mrow>
                  <mml:mtext>SW</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mi>a</mml:mi>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mi>Q</mml:mi>
                <mml:mrow>
                  <mml:mrow>
                    <mml:mn>1</mml:mn>
                    <mml:mo>/</mml:mo>
                    <mml:mn>2</mml:mn>
                  </mml:mrow>
                </mml:mrow>
              </mml:msup>
              <mml:mo>=</mml:mo>
              <mml:mn>1.54</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mn>6</mml:mn>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>m</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>The maximum mass and density are:</p>
        <disp-formula id="FD21">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>M</mml:mi>
                <mml:mrow>
                  <mml:mtext>SW</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mn>4</mml:mn>
              <mml:mi>π</mml:mi>
              <mml:msub>
                <mml:mi>m</mml:mi>
                <mml:mn>0</mml:mn>
              </mml:msub>
              <mml:mo>×</mml:mo>
              <mml:mi>Q</mml:mi>
              <mml:mo>=</mml:mo>
              <mml:mn>1.19</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mn>13</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>kg</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <disp-formula id="FD22">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>ρ</mml:mi>
                <mml:mrow>
                  <mml:mtext>SW</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mn>3</mml:mn>
              <mml:msub>
                <mml:mi>ρ</mml:mi>
                <mml:mn>0</mml:mn>
              </mml:msub>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mi>Q</mml:mi>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mrow>
                    <mml:mn>1</mml:mn>
                    <mml:mo>/</mml:mo>
                    <mml:mn>2</mml:mn>
                  </mml:mrow>
                </mml:mrow>
              </mml:msup>
              <mml:mo>=</mml:mo>
              <mml:mn>7.74</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>7</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>kg</mml:mtext>
              <mml:mo>⋅</mml:mo>
              <mml:msup>
                <mml:mtext>m</mml:mtext>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>3</mml:mn>
                </mml:mrow>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>Within this framework:</p>
        <p>Ball Lightning → Small Body SB1[<xref ref-type="bibr" rid="B1">1</xref>]Tunguska Superbolide → Small Body SB2 [<xref ref-type="bibr" rid="B2">2</xref>]C/2025 N1 (ATLAS) → Small Body SB3</p>
        <p>Thus, C/2025 N1 (ATLAS) is interpreted as a higher-order Small Body SB3, whose anomalous dynamics arise from internal processes associated with UCM Nucleus.</p>
        <p>Notably, the concept of superweak interactions was also explored by Wolfenstein [<xref ref-type="bibr" rid="B13">13</xref>], providing partial conceptual precedent.</p>
      </sec>
      <sec id="sec5dot5">
        <title>5.5. Micro-World (Weak Interaction)</title>
        <p>The Micro-world is governed by an interaction approximately 30 orders of magnitude stronger than gravity, with range:</p>
        <disp-formula id="FD23">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>R</mml:mi>
                <mml:mtext>W</mml:mtext>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mi>a</mml:mi>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mi>Q</mml:mi>
                <mml:mrow>
                  <mml:mrow>
                    <mml:mn>1</mml:mn>
                    <mml:mo>/</mml:mo>
                    <mml:mn>4</mml:mn>
                  </mml:mrow>
                </mml:mrow>
              </mml:msup>
              <mml:mo>=</mml:mo>
              <mml:mn>1.65</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>4</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>m</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>This scale is many orders of magnitude larger than the conventional weak nuclear force range, implying a fundamentally different interaction regime.</p>
        <p>The maximum mass is:</p>
        <disp-formula id="FD24">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>M</mml:mi>
                <mml:mtext>W</mml:mtext>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mn>4</mml:mn>
              <mml:mi>π</mml:mi>
              <mml:msub>
                <mml:mi>m</mml:mi>
                <mml:mn>0</mml:mn>
              </mml:msub>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mi>Q</mml:mi>
                <mml:mrow>
                  <mml:mrow>
                    <mml:mn>1</mml:mn>
                    <mml:mo>/</mml:mo>
                    <mml:mn>2</mml:mn>
                  </mml:mrow>
                </mml:mrow>
              </mml:msup>
              <mml:mo>=</mml:mo>
              <mml:mn>1.37</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>7</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>kg</mml:mtext>
              <mml:mo>≈</mml:mo>
              <mml:mn>6.28</mml:mn>
              <mml:msub>
                <mml:mi>M</mml:mi>
                <mml:mrow>
                  <mml:mtext>Pl</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>,</mml:mo>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>and the density:</p>
        <disp-formula id="FD25">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>ρ</mml:mi>
                <mml:mtext>W</mml:mtext>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mn>3</mml:mn>
              <mml:msub>
                <mml:mi>ρ</mml:mi>
                <mml:mn>0</mml:mn>
              </mml:msub>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mi>Q</mml:mi>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mrow>
                    <mml:mn>1</mml:mn>
                    <mml:mo>/</mml:mo>
                    <mml:mn>4</mml:mn>
                  </mml:mrow>
                </mml:mrow>
              </mml:msup>
              <mml:mo>=</mml:mo>
              <mml:mn>7.23</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mn>3</mml:mn>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>kg</mml:mtext>
              <mml:mo>⋅</mml:mo>
              <mml:msup>
                <mml:mtext>m</mml:mtext>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>3</mml:mn>
                </mml:mrow>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>Micro-world objects, with masses about the Planck mass <inline-formula><mml:math><mml:mrow><mml:msub><mml:mi> M </mml:mi><mml:mrow><mml:mtext> Pl </mml:mtext></mml:mrow></mml:msub></mml:mrow></mml:math></inline-formula> (including dust particles), are proposed as fundamental building blocks of all macroscopic structures.</p>
      </sec>
      <sec id="sec5dot6">
        <title>5.6. Cosmic Bubbles</title>
        <p>All four regimes—Macro, Large, Small, and Micro—are interpreted as Cosmic Bubbles with boundaries characterized by a universal surface energy density:</p>
        <disp-formula id="FD26">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>σ</mml:mi>
                <mml:mn>0</mml:mn>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mrow>
                <mml:mrow>
                  <mml:mi>h</mml:mi>
                  <mml:mi>c</mml:mi>
                </mml:mrow>
                <mml:mo>/</mml:mo>
                <mml:mrow>
                  <mml:msup>
                    <mml:mi>a</mml:mi>
                    <mml:mn>3</mml:mn>
                  </mml:msup>
                </mml:mrow>
              </mml:mrow>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>The total energy <inline-formula><mml:math><mml:mrow><mml:msub><mml:mi> E </mml:mi><mml:mrow><mml:mtext> CB </mml:mtext></mml:mrow></mml:msub></mml:mrow></mml:math></inline-formula> of a Cosmic Bubble of radius <inline-formula><mml:math><mml:mrow><mml:msub><mml:mi> R </mml:mi><mml:mrow><mml:mtext> CB </mml:mtext></mml:mrow></mml:msub></mml:mrow></mml:math></inline-formula> is [<xref ref-type="bibr" rid="B14">14</xref>]:</p>
        <disp-formula id="FD27">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>E</mml:mi>
                <mml:mrow>
                  <mml:mtext>CB</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mn>4</mml:mn>
              <mml:mi>π</mml:mi>
              <mml:msub>
                <mml:mi>σ</mml:mi>
                <mml:mn>0</mml:mn>
              </mml:msub>
              <mml:msubsup>
                <mml:mi>R</mml:mi>
                <mml:mrow>
                  <mml:mtext>CB</mml:mtext>
                </mml:mrow>
                <mml:mn>2</mml:mn>
              </mml:msubsup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>This relation provides a unifying description of structure formation across all scales, linking geometry, energy, and interaction strength.</p>
      </sec>
    </sec>
    <sec id="sec6">
      <title>6. Orbital Parameters of Solar System Bodies</title>
      <p>In celestial mechanics, there is no sharply defined maximum cometary aphelion, as long-period orbits are highly sensitive to perturbations and observational uncertainties. Nevertheless, empirical evidence suggests a practical upper limit of order</p>
      <disp-formula id="FD28">
        <mml:math>
          <mml:mrow>
            <mml:msub>
              <mml:mi>R</mml:mi>
              <mml:mrow>
                <mml:mtext>max</mml:mtext>
              </mml:mrow>
            </mml:msub>
            <mml:mo>~</mml:mo>
            <mml:msup>
              <mml:mrow>
                <mml:mn>10</mml:mn>
              </mml:mrow>
              <mml:mn>5</mml:mn>
            </mml:msup>
            <mml:mtext>
               
            </mml:mtext>
            <mml:mtext>AU</mml:mtext>
            <mml:mo>≈</mml:mo>
            <mml:mn>1.6</mml:mn>
            <mml:mtext>
               
            </mml:mtext>
            <mml:mtext>ly</mml:mtext>
            <mml:mo>,</mml:mo>
          </mml:mrow>
        </mml:math>
      </disp-formula>
      <p>as illustrated by the comets listed in <bold>Table 1</bold>.</p>
      <sec id="sec6dot1">
        <title>6.1. Solar System Hill Sphere (Galactic Context)</title>
        <p>The Hill sphere defines the region within which the gravitational influence of a system dominates over external tidal forces. For SS embedded in the Milky Way, the Hill radius <inline-formula><mml:math><mml:mrow><mml:msub><mml:mi> R </mml:mi><mml:mi> H </mml:mi></mml:msub></mml:mrow></mml:math></inline-formula> can be approximated as</p>
        <disp-formula id="FD29">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>R</mml:mi>
                <mml:mi>H</mml:mi>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:msub>
                <mml:mi>R</mml:mi>
                <mml:mrow>
                  <mml:mtext>GC</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:msup>
                <mml:mrow>
                  <mml:mrow>
                    <mml:mo>(</mml:mo>
                    <mml:mrow>
                      <mml:mfrac>
                        <mml:mrow>
                          <mml:msub>
                            <mml:mi>M</mml:mi>
                            <mml:mrow>
                              <mml:mtext>SS</mml:mtext>
                            </mml:mrow>
                          </mml:msub>
                        </mml:mrow>
                        <mml:mrow>
                          <mml:mn>3</mml:mn>
                          <mml:msub>
                            <mml:mi>M</mml:mi>
                            <mml:mrow>
                              <mml:mtext>MW</mml:mtext>
                            </mml:mrow>
                          </mml:msub>
                        </mml:mrow>
                      </mml:mfrac>
                    </mml:mrow>
                    <mml:mo>)</mml:mo>
                  </mml:mrow>
                </mml:mrow>
                <mml:mrow>
                  <mml:mrow>
                    <mml:mn>1</mml:mn>
                    <mml:mo>/</mml:mo>
                    <mml:mn>3</mml:mn>
                  </mml:mrow>
                </mml:mrow>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>where:</p>
        <p><inline-formula><mml:math><mml:mrow><mml:msub><mml:mi> R </mml:mi><mml:mrow><mml:mtext> GC </mml:mtext></mml:mrow></mml:msub><mml:mo> ≈ </mml:mo><mml:mn> 26.7 </mml:mn><mml:mtext>   </mml:mtext><mml:mtext> kly </mml:mtext></mml:mrow></mml:math></inline-formula> is the Galactocentric distance of the Sun<inline-formula><mml:math><mml:mrow><mml:msub><mml:mi> M </mml:mi><mml:mrow><mml:mtext> SS </mml:mtext></mml:mrow></mml:msub><mml:mo> ≈ </mml:mo><mml:mn> 2 </mml:mn><mml:mo> × </mml:mo><mml:msup><mml:mrow><mml:mn> 10 </mml:mn></mml:mrow><mml:mrow><mml:mn> 30 </mml:mn></mml:mrow></mml:msup><mml:mtext>   </mml:mtext><mml:mtext> kg </mml:mtext></mml:mrow></mml:math></inline-formula> is the SS mass<inline-formula><mml:math><mml:mrow><mml:msub><mml:mi> M </mml:mi><mml:mrow><mml:mtext> MW </mml:mtext></mml:mrow></mml:msub><mml:mo> ≈ </mml:mo><mml:mn> 1.15 </mml:mn><mml:mo> × </mml:mo><mml:msup><mml:mrow><mml:mn> 10 </mml:mn></mml:mrow><mml:mrow><mml:mn> 12 </mml:mn></mml:mrow></mml:msup><mml:msub><mml:mi> M </mml:mi><mml:mo> ⊙ </mml:mo></mml:msub></mml:mrow></mml:math></inline-formula> is the enclosed Galactic mass</p>
        <p>This yields</p>
        <disp-formula id="FD30">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>R</mml:mi>
                <mml:mi>H</mml:mi>
              </mml:msub>
              <mml:mo>≈</mml:mo>
              <mml:mn>1.67</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mn>16</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>m</mml:mtext>
              <mml:mo>≈</mml:mo>
              <mml:mn>1.11</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mn>5</mml:mn>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>AU</mml:mtext>
              <mml:mo>≈</mml:mo>
              <mml:mn>1.76</mml:mn>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>ly</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>The characteristic Large-world scale is</p>
        <disp-formula id="FD31">
          <mml:math display="inline">
            <mml:mrow>
              <mml:msub>
                <mml:mi>R</mml:mi>
                <mml:mrow>
                  <mml:mtext>EW</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mn>1.44</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mn>16</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>m</mml:mtext>
              <mml:mo>≈</mml:mo>
              <mml:mn>0.963</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mn>5</mml:mn>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>AU</mml:mtext>
              <mml:mo>≈</mml:mo>
              <mml:mn>1.52</mml:mn>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>ly</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>The close agreement between <inline-formula><mml:math><mml:mrow><mml:msub><mml:mi> R </mml:mi><mml:mi> H </mml:mi></mml:msub></mml:mrow></mml:math></inline-formula> and <inline-formula><mml:math><mml:mrow><mml:msub><mml:mi> R </mml:mi><mml:mrow><mml:mtext> EW </mml:mtext></mml:mrow></mml:msub></mml:mrow></mml:math></inline-formula> suggests that:</p>
        <p>the outer boundary of the Oort Cloud lies near ~10<sup>5</sup> AUstable cometary aphelia significantly beyond this scale are dynamically disfavored</p>
        <p>The corresponding maximum orbital period is</p>
        <disp-formula id="FD32">
          <mml:math>
            <mml:mrow>
              <mml:mi>T</mml:mi>
              <mml:mo>=</mml:mo>
              <mml:msqrt>
                <mml:mrow>
                  <mml:mfrac>
                    <mml:mrow>
                      <mml:msup>
                        <mml:mi>π</mml:mi>
                        <mml:mn>2</mml:mn>
                      </mml:msup>
                      <mml:msubsup>
                        <mml:mi>R</mml:mi>
                        <mml:mrow>
                          <mml:mtext>EW</mml:mtext>
                        </mml:mrow>
                        <mml:mn>3</mml:mn>
                      </mml:msubsup>
                    </mml:mrow>
                    <mml:mrow>
                      <mml:mn>2</mml:mn>
                      <mml:mi>G</mml:mi>
                      <mml:msub>
                        <mml:mi>M</mml:mi>
                        <mml:mo>⊙</mml:mo>
                      </mml:msub>
                    </mml:mrow>
                  </mml:mfrac>
                </mml:mrow>
              </mml:msqrt>
              <mml:mo>≈</mml:mo>
              <mml:mn>15</mml:mn>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>Myr</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>consistent with longest reliably determined periods of long-period comets (<bold>Table 1</bold>).</p>
        <p>The extremely large aphelion (~380,000 AU) and orbital period (~83 Myr) sometimes reported for C/2023 A3 (Tsuchinshan-ATLAS) are likely influenced by:</p>
        <p>observational uncertaintiesnon-gravitational perturbations</p>
        <p>For comparison, the distance to Proxima Centauri (≈ 4.24 ly) highlights that such orbital solutions approach interstellar scales.</p>
        <p>In standard astrophysics, the SS boundary is often associated with the Heliopause (~120 AU). In contrast, within the present framework the effective boundary is set by the Large-world scale (~10<sup>5</sup> AU), consistent with the observed cutoff in comet aphelia.</p>
        <p>No Solar System comet has a securely determined original barycentric aphelion exceeding ~10<sup>5</sup> AU; larger formal values arise naturally from uncertainties in near-parabolic orbit solutions.</p>
      </sec>
      <sec id="sec6dot2">
        <title>6.2. Motion with Non-Gravitational Acceleration</title>
        <p>To examine the dynamical impact of sustained NGA, consider radial motion under solar gravity plus a constant outward acceleration <inline-formula><mml:math><mml:mrow><mml:msub><mml:mi> a </mml:mi><mml:mrow><mml:mtext> NG </mml:mtext></mml:mrow></mml:msub></mml:mrow></mml:math></inline-formula> :</p>
        <disp-formula id="FD33">
          <mml:math>
            <mml:mrow>
              <mml:mfrac>
                <mml:mrow>
                  <mml:msup>
                    <mml:mtext>d</mml:mtext>
                    <mml:mn>2</mml:mn>
                  </mml:msup>
                  <mml:mi>r</mml:mi>
                </mml:mrow>
                <mml:mrow>
                  <mml:mtext>d</mml:mtext>
                  <mml:msup>
                    <mml:mi>t</mml:mi>
                    <mml:mn>2</mml:mn>
                  </mml:msup>
                </mml:mrow>
              </mml:mfrac>
              <mml:mo>=</mml:mo>
              <mml:mo>−</mml:mo>
              <mml:mfrac>
                <mml:mrow>
                  <mml:mi>G</mml:mi>
                  <mml:msub>
                    <mml:mi>M</mml:mi>
                    <mml:mo>⊙</mml:mo>
                  </mml:msub>
                </mml:mrow>
                <mml:mrow>
                  <mml:msup>
                    <mml:mi>r</mml:mi>
                    <mml:mn>2</mml:mn>
                  </mml:msup>
                </mml:mrow>
              </mml:mfrac>
              <mml:mo>+</mml:mo>
              <mml:msub>
                <mml:mi>a</mml:mi>
                <mml:mrow>
                  <mml:mtext>NG</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>,</mml:mo>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>with initial condition</p>
        <disp-formula id="FD34">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mrow>
                  <mml:mrow>
                    <mml:mrow>
                      <mml:mfrac>
                        <mml:mrow>
                          <mml:mtext>d</mml:mtext>
                          <mml:mi>r</mml:mi>
                        </mml:mrow>
                        <mml:mrow>
                          <mml:mtext>d</mml:mtext>
                          <mml:mi>t</mml:mi>
                        </mml:mrow>
                      </mml:mfrac>
                    </mml:mrow>
                    <mml:mo>|</mml:mo>
                  </mml:mrow>
                </mml:mrow>
                <mml:mrow>
                  <mml:mi>r</mml:mi>
                  <mml:mo>=</mml:mo>
                  <mml:msub>
                    <mml:mi>r</mml:mi>
                    <mml:mn>0</mml:mn>
                  </mml:msub>
                </mml:mrow>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:msub>
                <mml:mi>v</mml:mi>
                <mml:mn>0</mml:mn>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mn>0.</mml:mn>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>Integration yields</p>
        <disp-formula id="FD35">
          <mml:math>
            <mml:mrow>
              <mml:msup>
                <mml:mi>v</mml:mi>
                <mml:mn>2</mml:mn>
              </mml:msup>
              <mml:mo>=</mml:mo>
              <mml:mn>2</mml:mn>
              <mml:mrow>
                <mml:mo>[</mml:mo>
                <mml:mrow>
                  <mml:mi>G</mml:mi>
                  <mml:msub>
                    <mml:mi>M</mml:mi>
                    <mml:mo>⊙</mml:mo>
                  </mml:msub>
                  <mml:mrow>
                    <mml:mo>(</mml:mo>
                    <mml:mrow>
                      <mml:mfrac>
                        <mml:mn>1</mml:mn>
                        <mml:mi>r</mml:mi>
                      </mml:mfrac>
                      <mml:mo>−</mml:mo>
                      <mml:mfrac>
                        <mml:mn>1</mml:mn>
                        <mml:mrow>
                          <mml:msub>
                            <mml:mi>r</mml:mi>
                            <mml:mn>0</mml:mn>
                          </mml:msub>
                        </mml:mrow>
                      </mml:mfrac>
                    </mml:mrow>
                    <mml:mo>)</mml:mo>
                  </mml:mrow>
                  <mml:mo>+</mml:mo>
                  <mml:msub>
                    <mml:mi>a</mml:mi>
                    <mml:mrow>
                      <mml:mtext>NG</mml:mtext>
                    </mml:mrow>
                  </mml:msub>
                  <mml:mrow>
                    <mml:mo>(</mml:mo>
                    <mml:mrow>
                      <mml:msub>
                        <mml:mi>r</mml:mi>
                        <mml:mn>0</mml:mn>
                      </mml:msub>
                      <mml:mo>−</mml:mo>
                      <mml:mi>r</mml:mi>
                    </mml:mrow>
                    <mml:mo>)</mml:mo>
                  </mml:mrow>
                </mml:mrow>
                <mml:mo>]</mml:mo>
              </mml:mrow>
              <mml:mo>.</mml:mo>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>For <inline-formula><mml:math><mml:mrow><mml:mi> r </mml:mi><mml:mo> ≪ </mml:mo><mml:msub><mml:mi> r </mml:mi><mml:mn> 0 </mml:mn></mml:msub></mml:mrow></mml:math></inline-formula> , this simplifies to</p>
        <disp-formula id="FD36">
          <mml:math>
            <mml:mrow>
              <mml:msup>
                <mml:mi>v</mml:mi>
                <mml:mn>2</mml:mn>
              </mml:msup>
              <mml:mo>≈</mml:mo>
              <mml:mn>2</mml:mn>
              <mml:mrow>
                <mml:mo>(</mml:mo>
                <mml:mrow>
                  <mml:mfrac>
                    <mml:mrow>
                      <mml:mi>G</mml:mi>
                      <mml:msub>
                        <mml:mi>M</mml:mi>
                        <mml:mo>⊙</mml:mo>
                      </mml:msub>
                    </mml:mrow>
                    <mml:mi>r</mml:mi>
                  </mml:mfrac>
                  <mml:mo>+</mml:mo>
                  <mml:msub>
                    <mml:mi>a</mml:mi>
                    <mml:mrow>
                      <mml:mtext>NG</mml:mtext>
                    </mml:mrow>
                  </mml:msub>
                  <mml:msub>
                    <mml:mi>r</mml:mi>
                    <mml:mn>0</mml:mn>
                  </mml:msub>
                </mml:mrow>
                <mml:mo>)</mml:mo>
              </mml:mrow>
              <mml:mo>.</mml:mo>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>Taking the perihelion distance</p>
        <disp-formula id="FD37">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>r</mml:mi>
                <mml:mi>p</mml:mi>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mn>1.35645</mml:mn>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>AU</mml:mtext>
              <mml:mo>≈</mml:mo>
              <mml:mn>2.03</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mn>11</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>m</mml:mtext>
              <mml:mo>,</mml:mo>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>the gravitational contribution alone yields</p>
        <disp-formula id="FD38">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>v</mml:mi>
                <mml:mrow>
                  <mml:mtext>grav</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>≈</mml:mo>
              <mml:mn>3.62</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mn>4</mml:mn>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>m</mml:mtext>
              <mml:mo>⋅</mml:mo>
              <mml:msup>
                <mml:mtext>s</mml:mtext>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>1</mml:mn>
                </mml:mrow>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>The observed maximum velocity is</p>
        <disp-formula id="FD39">
          <mml:math display="inline">
            <mml:mrow>
              <mml:msub>
                <mml:mi>v</mml:mi>
                <mml:mrow>
                  <mml:mtext>max</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>≈</mml:mo>
              <mml:mn>6.83</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mn>4</mml:mn>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>m</mml:mtext>
              <mml:mo>⋅</mml:mo>
              <mml:msup>
                <mml:mtext>s</mml:mtext>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>1</mml:mn>
                </mml:mrow>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>Thus, the excess component satisfies</p>
        <disp-formula id="FD40">
          <mml:math>
            <mml:mrow>
              <mml:msubsup>
                <mml:mi>v</mml:mi>
                <mml:mrow>
                  <mml:mtext>NG</mml:mtext>
                </mml:mrow>
                <mml:mn>2</mml:mn>
              </mml:msubsup>
              <mml:mo>=</mml:mo>
              <mml:msubsup>
                <mml:mi>v</mml:mi>
                <mml:mrow>
                  <mml:mi>max</mml:mi>
                </mml:mrow>
                <mml:mn>2</mml:mn>
              </mml:msubsup>
              <mml:mo>−</mml:mo>
              <mml:msubsup>
                <mml:mi>v</mml:mi>
                <mml:mrow>
                  <mml:mtext>grav</mml:mtext>
                </mml:mrow>
                <mml:mn>2</mml:mn>
              </mml:msubsup>
              <mml:mo>≈</mml:mo>
              <mml:mn>3.36</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mn>9</mml:mn>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:msup>
                <mml:mtext>m</mml:mtext>
                <mml:mn>2</mml:mn>
              </mml:msup>
              <mml:mo>⋅</mml:mo>
              <mml:msup>
                <mml:mtext>s</mml:mtext>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>2</mml:mn>
                </mml:mrow>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>Assuming the NGA acts over a characteristic distance comparable to the Large-world scale,</p>
        <disp-formula id="FD41">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>r</mml:mi>
                <mml:mn>0</mml:mn>
              </mml:msub>
              <mml:mo>≈</mml:mo>
              <mml:msub>
                <mml:mi>R</mml:mi>
                <mml:mrow>
                  <mml:mtext>EW</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mn>1.44</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mn>16</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>m</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>we obtain</p>
        <disp-formula id="FD42">
          <mml:math display="inline">
            <mml:mrow>
              <mml:msub>
                <mml:mi>a</mml:mi>
                <mml:mrow>
                  <mml:mtext>NG</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>≈</mml:mo>
              <mml:mfrac>
                <mml:mrow>
                  <mml:msubsup>
                    <mml:mi>v</mml:mi>
                    <mml:mrow>
                      <mml:mtext>NG</mml:mtext>
                    </mml:mrow>
                    <mml:mn>2</mml:mn>
                  </mml:msubsup>
                </mml:mrow>
                <mml:mrow>
                  <mml:mn>2</mml:mn>
                  <mml:msub>
                    <mml:mi>r</mml:mi>
                    <mml:mn>0</mml:mn>
                  </mml:msub>
                </mml:mrow>
              </mml:mfrac>
              <mml:mo>≈</mml:mo>
              <mml:mn>1.17</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>7</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>m</mml:mtext>
              <mml:mo>⋅</mml:mo>
              <mml:msup>
                <mml:mtext>s</mml:mtext>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>2</mml:mn>
                </mml:mrow>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>This represents a lower bound, corresponding to acceleration acting over the maximum distance <inline-formula><mml:math><mml:mrow><mml:msub><mml:mi> r </mml:mi><mml:mn> 0 </mml:mn></mml:msub></mml:mrow></mml:math></inline-formula> . Even in this limiting case, the required acceleration lies at the upper end of—or exceeds—the typical range for cometary non-gravitational effects (10<sup>−</sup><sup>10</sup> − 10<sup>−7</sup> m∙<italic>s</italic><sup>−2</sup>).</p>
        <p>However, directly inferred values for C/2025 N1 (ATLAS) (Section 4.5) are of order</p>
        <disp-formula id="FD43">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>a</mml:mi>
                <mml:mrow>
                  <mml:mtext>NG</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>~</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>6</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>m</mml:mtext>
              <mml:mo>⋅</mml:mo>
              <mml:msup>
                <mml:mtext>s</mml:mtext>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>2</mml:mn>
                </mml:mrow>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>significantly exceeding expectations from standard outgassing models. We emphasize that the derived NGA is independent of the assumed initial velocity <inline-formula><mml:math><mml:mrow><mml:msub><mml:mi> v </mml:mi><mml:mn> 0 </mml:mn></mml:msub></mml:mrow></mml:math></inline-formula> . Consequently, an “interstellar body,” regardless of the value of <inline-formula><mml:math><mml:mrow><mml:msub><mml:mi> v </mml:mi><mml:mn> 0 </mml:mn></mml:msub></mml:mrow></mml:math></inline-formula> , cannot account for the directly inferred magnitude of <inline-formula><mml:math><mml:mrow><mml:msub><mml:mi> a </mml:mi><mml:mrow><mml:mtext> NG </mml:mtext></mml:mrow></mml:msub></mml:mrow></mml:math></inline-formula> .</p>
        <p>This analysis shows that:</p>
        <p>sustained NGA can significantly modify cometary velocitiesthe magnitude required for C/2025 N1 (ATLAS) exceeds that attainable by conventional mechanismsa fundamentally different physical process must therefore be considered</p>
        <p>Within the present framework, this is naturally interpreted as internal energy conversion, whereby rotational energy of the nucleus is transformed into translational kinetic energy of SB3.</p>
        <p>Moreover, weaker analogues of this process may contribute to the dynamics of other long-period comets, suggesting a broader role for NGA than traditionally assumed.</p>
      </sec>
      <sec id="sec6dot3">
        <title>6.3. Gravitationally Rounded Objects in the Solar System</title>
        <p>Within the present framework, all gravitationally rounded bodies—from planets to galaxy clusters—are proposed to contain cores composed of Universe-Created Matter (UCM). These cores consist of UCPs undergoing continuous self-annihilation, forming Self-Annihilating Reactors (SARs) that function as persistent internal energy sources.</p>
        <p>A representative lower bound for gravitationally rounded in SS is Saturn’s moon Mimas, with:</p>
        <p>Mean radius: 198.2 km ± 0.4 kmMass: 3.75 × 10<sup>19</sup> kgMean density: ∼1.15 × 10<sup>3</sup> kg∙m<sup>−3</sup>Surface temperature: ~ 64 K</p>
        <p>The observed temperature exceeds that expected from solar heating alone. Within the present framework, this discrepancy is attributed to internal energy generation within the UCM core. Even at relatively low densities (~10<sup>3</sup> kg∙m<sup>−3</sup>), self-annihilation processes may remain effective.</p>
        <p>Extending this concept, SARs are proposed to operate in all planetary bodies, including Earth, providing energy for:</p>
        <p>volcanismseismic activitylong-term geological evolution</p>
      </sec>
      <sec id="sec6dot4">
        <title>6.4. Tunguska Superbolide</title>
        <p>The Tunguska event is commonly interpreted as the atmospheric disruption of a ~50 - 60 m body, releasing ~3 - 30 Mt TNT equivalent at an altitude of ~5 - 10 km without forming an impact crater. Such events belong to the class of airbursts (fireballs or bolides), with the most energetic classified as superbolides.</p>
        <p>Meteoroids enter Earth’s atmosphere at velocities ≥ 11 km/s, compressing the air ahead of them and generating extreme temperatures through adiabatic heating (ram pressure). This process leads to ablation, fragmentation, or explosive disruption.</p>
        <p><bold>WUC Interpretati</bold><bold>on</bold></p>
        <p>The Tunguska object (SB2) is interpreted as follows:</p>
        <p>It possessed a low-density UCM core (&lt;10<sup>3</sup> kg∙m<sup>−3</sup>).Under normal conditions, self-annihilation was inefficient, allowing stability in space.Atmospheric entry increased core density via ram pressure.A critical threshold triggered rapid self-annihilation, producing explosive energy release.</p>
        <p>The estimated maximum energy</p>
        <disp-formula id="FD44">
          <mml:math display="inline">
            <mml:mrow>
              <mml:msub>
                <mml:mi>E</mml:mi>
                <mml:mrow>
                  <mml:mtext>SB</mml:mtext>
                  <mml:mn>2</mml:mn>
                </mml:mrow>
              </mml:msub>
              <mml:mo>≈</mml:mo>
              <mml:mn>1.26</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mn>17</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>J</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>implies a core volume</p>
        <disp-formula id="FD45">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>V</mml:mi>
                <mml:mrow>
                  <mml:mtext>core</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>≈</mml:mo>
              <mml:mn>0.4</mml:mn>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:msup>
                <mml:mtext>m</mml:mtext>
                <mml:mn>3</mml:mn>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>corresponding to a characteristic diameter</p>
        <disp-formula id="FD46">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>D</mml:mi>
                <mml:mrow>
                  <mml:mtext>core</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>~</mml:mo>
              <mml:mn>1</mml:mn>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>m</mml:mtext>
              <mml:mo>.</mml:mo>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>Thus, SB2 bodies are interpreted as metastable UCM structures capable of rapid energy release under external perturbations.</p>
      </sec>
    </sec>
    <sec id="sec7">
      <title>7. Solar System Small Bodies</title>
      <sec id="sec7dot1">
        <title>7.1. Origin of Solar System Small Bodies</title>
        <p>In the present framework, Ecliptic Small Bodies (SBs) were produced by the Sun as the result of Volcanic Rotational Fission (VRF) of the Sun’s UCM Core 4.57 Byr ago [<xref ref-type="bibr" rid="B1">1</xref>].</p>
        <p>Nearly isotropic SBs were produced by Giant Planets with different directions of their rotational axes (which are, in fact, “Failed stars”) as the result of VRF of their UCM cores 4.57 Byr ago.</p>
        <p>UCM cores of satellite objects can be any size from micrometers to thousands of km. Satellites are rocky or icy bodies as the result of the self-annihilation of UCPs inside of their cores with a density ≳ 10<sup>3</sup> kg∙m<sup>−3</sup>.</p>
        <p>All chemical elements, compositions, and radiative outputs are generated in situ through UCP self-annihilation within UCM cores of asteroids and comets. The formation of all objects in SS has a good explanation.</p>
        <p>In case when the density of UCM cores of satellites is &lt;10<sup>3</sup> kg∙m<sup>−3</sup>, the self-annihilation process is not efficient. Then, there is a possibility of stable UCM Bolides (SB2), which are the analog of Ball Lightnings (SB1) with much larger internal energy.</p>
      </sec>
      <sec id="sec7dot2">
        <title>7.2. Characteristics of Small Solar System Bodies</title>
        <p>SBs are governed by the super-weak interaction. Its characteristic interaction range is:</p>
        <disp-formula id="FD47">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>R</mml:mi>
                <mml:mrow>
                  <mml:mtext>SW</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mi>a</mml:mi>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mi>Q</mml:mi>
                <mml:mrow>
                  <mml:mrow>
                    <mml:mn>1</mml:mn>
                    <mml:mo>/</mml:mo>
                    <mml:mn>2</mml:mn>
                  </mml:mrow>
                </mml:mrow>
              </mml:msup>
              <mml:mo>≈</mml:mo>
              <mml:mn>1.54</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mn>3</mml:mn>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>km</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>The theoretical maximum Small-world mass is:</p>
        <disp-formula id="FD48">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>M</mml:mi>
                <mml:mrow>
                  <mml:mtext>SW</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mn>1.19</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mn>13</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>kg</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>SBs consist of Nuclei and Inner Comae. Nuclei are Rotating Balls made of UCM with density in the range from 3.44 kg∙m<sup>−3</sup> up to ~10<sup>3</sup> kg∙m<sup>−3</sup>, at different rotation speeds up to the maximum speed at the nucleus equator equals the escape velocity.</p>
        <p>The range of the weak interaction for particles UCF1 (1.3 TeV) is:</p>
        <disp-formula id="FD49">
          <mml:math>
            <mml:mrow>
              <mml:msubsup>
                <mml:mi>R</mml:mi>
                <mml:mrow>
                  <mml:mtext>UCF</mml:mtext>
                  <mml:mn>1</mml:mn>
                </mml:mrow>
                <mml:mi>W</mml:mi>
              </mml:msubsup>
              <mml:mo>=</mml:mo>
              <mml:mn>0.88</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>8</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>m</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>and a calculated minimum particle concentration is:</p>
        <disp-formula id="FD50">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>n</mml:mi>
                <mml:mrow>
                  <mml:mtext>UCF</mml:mtext>
                  <mml:mn>1</mml:mn>
                </mml:mrow>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mn>1.47</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mn>24</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:msup>
                <mml:mtext>m</mml:mtext>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>3</mml:mn>
                </mml:mrow>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>Considering the rest energy of UCF1:</p>
        <disp-formula id="FD51">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>E</mml:mi>
                <mml:mrow>
                  <mml:mtext>UCF</mml:mtext>
                  <mml:mn>1</mml:mn>
                </mml:mrow>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mn>1.315</mml:mn>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>TeV</mml:mtext>
              <mml:mo>=</mml:mo>
              <mml:mn>2.11</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>7</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>J</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>we can calculate the minimum energy density of the UCM core:</p>
        <disp-formula id="FD52">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>ρ</mml:mi>
                <mml:mrow>
                  <mml:mtext>UCF</mml:mtext>
                  <mml:mn>1</mml:mn>
                </mml:mrow>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mn>3.1</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mn>17</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mrow>
                <mml:mtext>J</mml:mtext>
                <mml:mo>/</mml:mo>
                <mml:mrow>
                  <mml:msup>
                    <mml:mtext>m</mml:mtext>
                    <mml:mn>3</mml:mn>
                  </mml:msup>
                </mml:mrow>
              </mml:mrow>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>that is equivalent to the mass density of 3.44 kg∙m<sup>−3</sup> that is not enough for efficient self-annihilation.</p>
        <p>Inner Comae have different diameters <inline-formula><mml:math><mml:mrow><mml:msub><mml:mi> D </mml:mi><mml:mrow><mml:mtext> IC </mml:mtext></mml:mrow></mml:msub></mml:mrow></mml:math></inline-formula> in the range of ~10<sup>3</sup> km up to the maximum diameter:</p>
        <disp-formula id="FD53">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>D</mml:mi>
                <mml:mrow>
                  <mml:mtext>IC</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mn>2</mml:mn>
              <mml:msub>
                <mml:mi>R</mml:mi>
                <mml:mrow>
                  <mml:mtext>SW</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>≈</mml:mo>
              <mml:mn>3.1</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mn>3</mml:mn>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>km</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p><bold>Micro-</bold><bold>World</bold><bold>Connection: Dust and Coma Formati</bold><bold>on</bold></p>
        <p>The weak-interaction scale:</p>
        <disp-formula id="FD54">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>R</mml:mi>
                <mml:mtext>W</mml:mtext>
              </mml:msub>
              <mml:mo>≈</mml:mo>
              <mml:mn>1.65</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>4</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>m</mml:mtext>
              <mml:mo>≈</mml:mo>
              <mml:mn>165</mml:mn>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mi>μ</mml:mi>
              <mml:mtext>m</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>matches the observed diameters of large dust grains <inline-formula><mml:math><mml:mrow><mml:msub><mml:mi> D </mml:mi><mml:mrow><mml:mtext> DG </mml:mtext></mml:mrow></mml:msub></mml:mrow></mml:math></inline-formula> in the inner comae [<xref ref-type="bibr" rid="B15">15</xref>] up to the maximum diameter <inline-formula><mml:math display="inline"><mml:mrow><mml:msub><mml:mi> D </mml:mi><mml:mrow><mml:mi> max </mml:mi></mml:mrow></mml:msub></mml:mrow></mml:math></inline-formula> :</p>
        <disp-formula id="FD55">
          <mml:math display="inline">
            <mml:mrow>
              <mml:msub>
                <mml:mi>D</mml:mi>
                <mml:mrow>
                  <mml:mi>max</mml:mi>
                </mml:mrow>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mn>2</mml:mn>
              <mml:msub>
                <mml:mi>R</mml:mi>
                <mml:mtext>W</mml:mtext>
              </mml:msub>
              <mml:mo>≈</mml:mo>
              <mml:mn>330</mml:mn>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mi>μ</mml:mi>
              <mml:mtext>m</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>This suggests that:</p>
        <p>Micro-world objects (UCM fragments) are continuously generated due to the Rotational Fission of Nuclei made of UCM.These fragments evolve into dust grains and volatiles via UCP self-annihilation.The Inner comae are thus a direct manifestation of internal UCM processes.</p>
        <p><bold>Micro-Volcanism (MiV) Mechani</bold><bold>sm</bold></p>
        <p>The activity of SBs is driven by recurrent MiVs, governed by the following cycle:</p>
        <p><bold>1)</bold><bold>Energy Release Pha</bold><bold>se</bold></p>
        <p>The UCM core ejects material.A small fraction of mass is lost.A significant fraction of rotational angular momentum is dissipated.</p>
        <p><bold>2)</bold><bold>Accumulation Pha</bold><bold>se</bold></p>
        <p>The core continuously absorbs UCPs from the four-dimensional Nucleus of the World created by the Eternal Universe.Mass increases as <inline-formula><mml:math><mml:mrow><mml:mi> M </mml:mi><mml:mo> ∝ </mml:mo><mml:mi> τ </mml:mi></mml:mrow></mml:math></inline-formula> (cosmological time).Angular momentum increases faster <inline-formula><mml:math><mml:mrow><mml:mi> L </mml:mi><mml:mo> ∝ </mml:mo><mml:msup><mml:mi> τ </mml:mi><mml:mrow><mml:mrow><mml:mn> 3 </mml:mn><mml:mo> / </mml:mo><mml:mn> 2 </mml:mn></mml:mrow></mml:mrow></mml:msup></mml:mrow></mml:math></inline-formula> .</p>
        <p><bold>3)</bold><bold>Instability Thresho</bold><bold>ld</bold></p>
        <p>When the rotational velocity of the core approaches the escape velocity, a new MiV event is triggered.</p>
        <p><bold>4)</bold><bold>Continuous Outfl</bold><bold>ow</bold></p>
        <p>Dust grains and volatiles are continuously replenished.</p>
        <p><bold>Energy Conversion Mechani</bold><bold>sm</bold></p>
        <p>A key feature of the model is the conversion of rotational energy into translational kinetic energy:</p>
        <p>MiVs generate internal torques.These torques reduce the rotational energy of nuclei while increasing their translational kinetic energy.The process is analogous to a rotating body converting spin into linear motion under frictional interaction.</p>
        <p>This mechanism naturally explains:</p>
        <p>The large NGA.The enhanced perihelion velocity.The stability of NGA over time.</p>
        <p>Importantly, the Nucleus is assumed to rotate at a near-critical equatorial velocity, approximately equal to its escape velocity, maintaining a quasi-steady energy conversion regime.</p>
        <p><bold>Synthes</bold><bold>is</bold></p>
        <p>Within the present framework:</p>
        <p>C/2025 N1 (ATLAS) is interpreted as a Small Body (SB3).Its coma, dust production, and dynamics arise from internal UCM processes.Its anomalous trajectory is explained by continuous internal energy conversion, rather than external forces alone.</p>
        <p>This interpretation provides a unified explanation linking:</p>
        <p>Cometary activityNGAHyperbolic motion</p>
      </sec>
      <sec id="sec7dot3">
        <title>7.3. Nucleus of Small Body</title>
        <p>Estimates of the Nucleus properties of C/2025 N1 (ATLAS) are highly model-dependent. Reported values include [<xref ref-type="bibr" rid="B16">16</xref>]:</p>
        <p>Density: <inline-formula><mml:math><mml:mrow><mml:mi> ρ </mml:mi><mml:mo> ≈ </mml:mo><mml:mn> 200 </mml:mn><mml:mtext>   </mml:mtext><mml:mtext> - </mml:mtext><mml:mtext>   </mml:mtext><mml:mn> 600 </mml:mn><mml:mtext>   </mml:mtext><mml:mtext> kg </mml:mtext><mml:mo> ⋅ </mml:mo><mml:msup><mml:mtext> m </mml:mtext><mml:mrow><mml:mo> − </mml:mo><mml:mn> 3 </mml:mn></mml:mrow></mml:msup></mml:mrow></mml:math></inline-formula> Mass: <inline-formula><mml:math><mml:mrow><mml:mi> M </mml:mi><mml:mo> ≈ </mml:mo><mml:mn> 4.4 </mml:mn><mml:mo> × </mml:mo><mml:msup><mml:mrow><mml:mn> 10 </mml:mn></mml:mrow><mml:mrow><mml:mn> 10 </mml:mn></mml:mrow></mml:msup><mml:mtext>   </mml:mtext><mml:mtext> kg </mml:mtext></mml:mrow></mml:math></inline-formula> Diameter: <inline-formula><mml:math><mml:mrow><mml:mi> D </mml:mi><mml:mo> ≈ </mml:mo><mml:mn> 0.520 </mml:mn><mml:mtext>   </mml:mtext><mml:mtext> - </mml:mtext><mml:mtext>   </mml:mtext><mml:mtext> 0 </mml:mtext><mml:mn> .748 </mml:mn><mml:mtext>   </mml:mtext><mml:mtext> km </mml:mtext></mml:mrow></mml:math></inline-formula></p>
        <p>However, within the present framework, the only directly measured parameters are:</p>
        <p>Rotation period: <inline-formula><mml:math><mml:mrow><mml:mi> T </mml:mi><mml:mo> = </mml:mo><mml:mrow><mml:mo> ( </mml:mo><mml:mrow><mml:mn> 16.16 </mml:mn><mml:mo> ± </mml:mo><mml:mn> 0.01 </mml:mn></mml:mrow><mml:mo> ) </mml:mo></mml:mrow><mml:mtext> h </mml:mtext></mml:mrow></mml:math></inline-formula> Diameter (Hubble): <inline-formula><mml:math><mml:mrow><mml:msub><mml:mi> D </mml:mi><mml:mi> H </mml:mi></mml:msub><mml:mo> = </mml:mo><mml:mn> 0.32 </mml:mn><mml:mtext>   </mml:mtext><mml:mtext> - </mml:mtext><mml:mtext>   </mml:mtext><mml:mn> 5.6 </mml:mn><mml:mtext>   </mml:mtext><mml:mtext> km </mml:mtext></mml:mrow></mml:math></inline-formula></p>
        <p><bold>Rotation-Constrained Density</bold><inline-formula><mml:math display="inline"><mml:mi> ρ </mml:mi></mml:math></inline-formula></p>
        <p>Assuming that the equatorial velocity equals the escape velocity <inline-formula><mml:math><mml:mrow><mml:mi> v </mml:mi><mml:mo> = </mml:mo><mml:msub><mml:mi> v </mml:mi><mml:mrow><mml:mi> e </mml:mi><mml:mi> s </mml:mi><mml:mi> c </mml:mi></mml:mrow></mml:msub></mml:mrow></mml:math></inline-formula> , that is a condition for the production of dust grains due to the Rotational Fission of the nucleus made of Universe-Created Matter (UCM):</p>
        <disp-formula id="FD56">
          <mml:math>
            <mml:mrow>
              <mml:msup>
                <mml:mi>v</mml:mi>
                <mml:mn>2</mml:mn>
              </mml:msup>
              <mml:mo>=</mml:mo>
              <mml:mfrac>
                <mml:mrow>
                  <mml:mn>2</mml:mn>
                  <mml:mi>G</mml:mi>
                  <mml:mi>M</mml:mi>
                </mml:mrow>
                <mml:mi>R</mml:mi>
              </mml:mfrac>
              <mml:mo>=</mml:mo>
              <mml:mfrac>
                <mml:mrow>
                  <mml:mn>8</mml:mn>
                  <mml:mi>π</mml:mi>
                  <mml:mi>G</mml:mi>
                  <mml:mi>ρ</mml:mi>
                </mml:mrow>
                <mml:mn>3</mml:mn>
              </mml:mfrac>
              <mml:msup>
                <mml:mi>R</mml:mi>
                <mml:mn>2</mml:mn>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>we obtain:</p>
        <disp-formula id="FD57">
          <mml:math>
            <mml:mrow>
              <mml:mi>ω</mml:mi>
              <mml:mo>=</mml:mo>
              <mml:mfrac>
                <mml:mi>v</mml:mi>
                <mml:mi>R</mml:mi>
              </mml:mfrac>
              <mml:mo>=</mml:mo>
              <mml:msqrt>
                <mml:mrow>
                  <mml:mfrac>
                    <mml:mrow>
                      <mml:mn>8</mml:mn>
                      <mml:mi>π</mml:mi>
                      <mml:mi>G</mml:mi>
                      <mml:mi>ρ</mml:mi>
                    </mml:mrow>
                    <mml:mn>3</mml:mn>
                  </mml:mfrac>
                </mml:mrow>
              </mml:msqrt>
              <mml:mo>=</mml:mo>
              <mml:mfrac>
                <mml:mrow>
                  <mml:mn>2</mml:mn>
                  <mml:mi>π</mml:mi>
                </mml:mrow>
                <mml:mi>T</mml:mi>
              </mml:mfrac>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>This yields a density depending only on the rotation period:</p>
        <disp-formula id="FD58">
          <mml:math>
            <mml:mrow>
              <mml:mi>ρ</mml:mi>
              <mml:mo>=</mml:mo>
              <mml:mfrac>
                <mml:mrow>
                  <mml:mn>3</mml:mn>
                  <mml:mi>π</mml:mi>
                </mml:mrow>
                <mml:mrow>
                  <mml:mn>2</mml:mn>
                  <mml:mi>G</mml:mi>
                  <mml:msup>
                    <mml:mi>T</mml:mi>
                    <mml:mn>2</mml:mn>
                  </mml:msup>
                </mml:mrow>
              </mml:mfrac>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <disp-formula id="FD59">
          <mml:math>
            <mml:mrow>
              <mml:mi>T</mml:mi>
              <mml:mo>=</mml:mo>
              <mml:mn>16.16</mml:mn>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>h</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <disp-formula id="FD60">
          <mml:math>
            <mml:mrow>
              <mml:mi>ρ</mml:mi>
              <mml:mo>≈</mml:mo>
              <mml:mn>20.9</mml:mn>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>kg</mml:mtext>
              <mml:mo>⋅</mml:mo>
              <mml:msup>
                <mml:mtext>m</mml:mtext>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>3</mml:mn>
                </mml:mrow>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p><bold>Implicatio</bold><bold>ns</bold></p>
        <p><inline-formula><mml:math><mml:mrow><mml:mi> ρ </mml:mi><mml:mo> ≫ </mml:mo><mml:mn> 3.44 </mml:mn><mml:mtext>   </mml:mtext><mml:mtext> kg </mml:mtext><mml:mo> ⋅ </mml:mo><mml:msup><mml:mtext> m </mml:mtext><mml:mrow><mml:mo> − </mml:mo><mml:mn> 3 </mml:mn></mml:mrow></mml:msup></mml:mrow></mml:math></inline-formula> (minimum UCM core density)<inline-formula><mml:math display="inline"><mml:mrow><mml:mi> ρ </mml:mi><mml:mo> ≪ </mml:mo><mml:msup><mml:mrow><mml:mn> 10 </mml:mn></mml:mrow><mml:mn> 3 </mml:mn></mml:msup><mml:mtext>   </mml:mtext><mml:mtext> kg </mml:mtext><mml:mo> ⋅ </mml:mo><mml:msup><mml:mtext> m </mml:mtext><mml:mrow><mml:mo> − </mml:mo><mml:mn> 3 </mml:mn></mml:mrow></mml:msup></mml:mrow></mml:math></inline-formula> (efficient SAR threshold)</p>
        <p>Thus, the nucleus is long-term stable, with low-rate self-annihilation.</p>
        <p><bold>Size and Mass Constrain</bold><bold>ts</bold></p>
        <p>Maximum possible radius (using Small-world mass limit <inline-formula><mml:math><mml:mrow><mml:msub><mml:mi> M </mml:mi><mml:mrow><mml:mi> S </mml:mi><mml:mi> W </mml:mi></mml:mrow></mml:msub><mml:mo> = </mml:mo><mml:mn> 1.19 </mml:mn><mml:mo> × </mml:mo><mml:msup><mml:mrow><mml:mn> 10 </mml:mn></mml:mrow><mml:mrow><mml:mn> 13 </mml:mn></mml:mrow></mml:msup><mml:mtext>   </mml:mtext><mml:mtext> kg </mml:mtext></mml:mrow></mml:math></inline-formula> ):</p>
        <disp-formula id="FD61">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>R</mml:mi>
                <mml:mrow>
                  <mml:mtext>max</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>≈</mml:mo>
              <mml:mn>5.15</mml:mn>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>km</mml:mtext>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:msub>
                <mml:mi>D</mml:mi>
                <mml:mrow>
                  <mml:mtext>max</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>≈</mml:mo>
              <mml:mn>10.3</mml:mn>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>km</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>For the reported mass 4.4 × 10<sup>10</sup> kg:</p>
        <disp-formula id="FD62">
          <mml:math>
            <mml:mrow>
              <mml:mi>R</mml:mi>
              <mml:mo>≈</mml:mo>
              <mml:mn>0.80</mml:mn>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>km</mml:mtext>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mi>D</mml:mi>
              <mml:mo>≈</mml:mo>
              <mml:mn>1.6</mml:mn>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>km</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>Using the observational upper bound <inline-formula><mml:math><mml:mrow><mml:msub><mml:mi> R </mml:mi><mml:mi> H </mml:mi></mml:msub><mml:mo> ≤ </mml:mo><mml:mn> 2.8 </mml:mn><mml:mtext>   </mml:mtext><mml:mtext> km </mml:mtext></mml:mrow></mml:math></inline-formula> , the corresponding mass is:</p>
        <disp-formula id="FD63">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>M</mml:mi>
                <mml:mi>H</mml:mi>
              </mml:msub>
              <mml:mo>≲</mml:mo>
              <mml:mn>1.92</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mn>12</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>kg</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>These values define a physically consistent parameter space for the Nucleus.</p>
        <p><bold>Rotational Ener</bold><bold>gy</bold></p>
        <disp-formula id="FD64">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>R</mml:mi>
                <mml:mi>H</mml:mi>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mn>2.8</mml:mn>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>km</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <disp-formula id="FD65">
          <mml:math>
            <mml:mrow>
              <mml:mi>v</mml:mi>
              <mml:mo>=</mml:mo>
              <mml:mi>ω</mml:mi>
              <mml:msub>
                <mml:mi>R</mml:mi>
                <mml:mi>H</mml:mi>
              </mml:msub>
              <mml:mo>≈</mml:mo>
              <mml:mn>0.30</mml:mn>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>m</mml:mtext>
              <mml:mo>⋅</mml:mo>
              <mml:msup>
                <mml:mtext>s</mml:mtext>
                <mml:mrow>
                  <mml:mo>−</mml:mo>
                  <mml:mn>1</mml:mn>
                </mml:mrow>
              </mml:msup>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <disp-formula id="FD66">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>E</mml:mi>
                <mml:mrow>
                  <mml:mtext>rot</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mfrac>
                <mml:mn>1</mml:mn>
                <mml:mn>5</mml:mn>
              </mml:mfrac>
              <mml:mi>M</mml:mi>
              <mml:msup>
                <mml:mi>v</mml:mi>
                <mml:mn>2</mml:mn>
              </mml:msup>
              <mml:mo>≈</mml:mo>
              <mml:mn>3.5</mml:mn>
              <mml:mo>×</mml:mo>
              <mml:msup>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
                <mml:mrow>
                  <mml:mn>10</mml:mn>
                </mml:mrow>
              </mml:msup>
              <mml:mtext>
                 
              </mml:mtext>
              <mml:mtext>J</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>This rotational energy of the nucleus acts as a reservoir for conversion into translational kinetic energy of C/2025 N1 (ATLAS), contributing to the observed NGA.</p>
      </sec>
    </sec>
    <sec id="sec8">
      <title>8. WUC Explanation of C/2025 N1 (ATLAS) Observations</title>
      <sec id="sec8dot1">
        <title>8.1. Key Observations of C/2025 N1 (ATLAS)</title>
        <p>C/2025 N1 (ATLAS) appears distinctly diffuse in telescope images, indicating that its nucleus is surrounded by a coma—a cloud of gas and dust produced by outgassing. Coma maps of H<sub>2</sub>O, CO<sub>2</sub>, and CH<sub>4</sub> (<xref ref-type="fig" rid="fig1">Figure 1</xref>) reveal structured emission </p>
        <fig id="fig1">
          <label>Figure 1</label>
          <graphic xlink:href="https://html.scirp.org/file/2181625-rId291.jpeg?20260928014548" />
        </fig>
        <p><bold>Figure 1.</bold> Coma maps of H<sub>2</sub>O, CO<sub>2</sub>, and CH<sub>4</sub>, computed as the integrated emission flux across the corresponding fluorescence bands for Observations 6, 15, and 13, respectively. The sunward and target velocity directions are denoted by the white arrows. The target centroids, computed as the photocenter in the median-stacked images, are marked with the black points. For H<sub>2</sub>O and CO<sub>2</sub>, the white contours correspond to emission levels of 75%, 50%, and 25% relative to the maximum value and illustrate the slight anti-sunward extension of the respective comae. The precise spatial distribution of CH<sub>4</sub> in the near-nucleus region is poorly constrained due to the low signal-to-noise ratio of the data. Adapted from [<xref ref-type="bibr" rid="B17">17</xref>].</p>
        <p>with a modest anti-sunward extension. The inner coma has a characteristic scale of several thousand kilometers that is in good agreement with the observed data [<xref ref-type="bibr" rid="B17">17</xref>].</p>
        <p>Space-based imaging further confirms typical cometary morphology. Observations from ESA’s <italic>JUICE</italic> mission show a bright coma, extended tail, and fine structures including jets, filaments, and streams [<xref ref-type="bibr" rid="B18">18</xref>] (<xref ref-type="fig" rid="fig2">Figure 2</xref>). Although often described as an interstellar visitor, its observed behavior is consistent with that of an active comet.</p>
        <p>Ultraviolet observations obtained by NASA’s <italic>Europa Clipper</italic> spacecraft (<xref ref-type="fig" rid="fig3">Figure 3</xref>) reveal a compact UV-bright region near the nucleus, although its precise size remains unconstrained due to instrumental limitations [<xref ref-type="bibr" rid="B19">19</xref>].</p>
        <fig id="fig2">
          <label>Figure 2</label>
          <graphic xlink:href="https://html.scirp.org/file/2181625-rId292.jpeg?20260928014548" />
        </fig>
        <p><bold>Figure 2.</bold> The arrows in the top left indicate the direction in which the comet was moving (blue) and the relative direction of the Sun (yellow). Adapted from [<xref ref-type="bibr" rid="B18">18</xref>].</p>
        <fig id="fig3">
          <label>Figure 3</label>
          <graphic xlink:href="https://html.scirp.org/file/2181625-rId293.jpeg?20260928014548" />
        </fig>
        <p><bold>Figure 3.</bold> Interstellar comet 3I/ATLAS is seen in this composite image captured on Nov. 6, 2025, by the Europa Ultraviolet Spectrograph instrument on NASA’s Europa Clipper spacecraft, from a distance of around 103 million miles (164 million kilometers). Adapted from [<xref ref-type="bibr" rid="B19">19</xref>].</p>
        <p>X-ray observations by <italic>XMM</italic>-<italic>Newton</italic> and <italic>XRISM</italic> [<xref ref-type="bibr" rid="B20">20</xref>]-[<xref ref-type="bibr" rid="B22">22</xref>] (<xref ref-type="fig" rid="fig4">Figure 4</xref>) detect:</p>
        <p>extended emission in the 0.3 - 1.0 keV rangespatial scales up to ~ 4 × 10<sup>5</sup> kmspectral features associated with C, N, and O</p>
        <fig id="fig4">
          <label>Figure 4</label>
          <graphic xlink:href="https://html.scirp.org/file/2181625-rId294.jpeg?20260928014548" />
        </fig>
        <p><bold>Figure 4.</bold> An image of comet 3I/ATLAS from the X-Ray Imaging and Spectroscopy Mission (XRISM). Image credit: JAXA.</p>
        <p>These emissions are conventionally interpreted as solar wind charge exchange with neutral coma gas. Notably, X-ray diagnostics are particularly sensitive to hydrogen and nitrogen species that are difficult to detect at optical and infrared wavelengths.</p>
      </sec>
      <sec id="sec8dot2">
        <title>8.2. Cosmic-Ray Processing Signatures</title>
        <p>Spectroscopic observations using <italic>JWST</italic>/<italic>NIRSpec</italic> and <italic>SPHEREx</italic> reveal an unusually high CO<sub>2</sub> enrichment:</p>
        <disp-formula id="FD67">
          <mml:math>
            <mml:mrow>
              <mml:mrow>
                <mml:mrow>
                  <mml:msub>
                    <mml:mrow>
                      <mml:mtext>CO</mml:mtext>
                    </mml:mrow>
                    <mml:mn>2</mml:mn>
                  </mml:msub>
                </mml:mrow>
                <mml:mo>/</mml:mo>
                <mml:mrow>
                  <mml:msub>
                    <mml:mtext>H</mml:mtext>
                    <mml:mn>2</mml:mn>
                  </mml:msub>
                  <mml:mtext>O</mml:mtext>
                </mml:mrow>
              </mml:mrow>
              <mml:mo>=</mml:mo>
              <mml:mn>7.6</mml:mn>
              <mml:mo>±</mml:mo>
              <mml:mn>0.3</mml:mn>
              <mml:mo>,</mml:mo>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>significantly exceeding typical SS comet values [<xref ref-type="bibr" rid="B23">23</xref>]. Elevated CO abundance</p>
        <disp-formula id="FD68">
          <mml:math>
            <mml:mrow>
              <mml:mrow>
                <mml:mrow>
                  <mml:mtext>CO</mml:mtext>
                </mml:mrow>
                <mml:mo>/</mml:mo>
                <mml:mrow>
                  <mml:msub>
                    <mml:mtext>H</mml:mtext>
                    <mml:mn>2</mml:mn>
                  </mml:msub>
                  <mml:mtext>O</mml:mtext>
                </mml:mrow>
              </mml:mrow>
              <mml:mo>=</mml:mo>
              <mml:mn>1.65</mml:mn>
              <mml:mo>±</mml:mo>
              <mml:mn>0.09</mml:mn>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>and pronounced red spectral slopes further characterize the object [<xref ref-type="bibr" rid="B24">24</xref>].</p>
        <p>In standard interpretations, this composition is attributed to galactic cosmic ray processing of surface layers. Laboratory studies show that irradiation can convert CO into CO<sub>2</sub> and produce organic-rich crusts. The observed outgassing is therefore thought to sample only a shallow processed layer (~15 - 20 m), rather than pristine interior material.</p>
        <p>This interpretation implies that long-residence interstellar objects primarily expose radiation-processed material rather than original formation signatures.</p>
      </sec>
      <sec id="sec8dot3">
        <title>8.3. Coma Composition and Dust Properties</title>
        <p>The coma of C/2025 N1 (ATLAS) exhibits:</p>
        <p>strong and evolving outgassing (e.g., [<xref ref-type="bibr" rid="B25">25</xref>]-[<xref ref-type="bibr" rid="B28">28</xref>])dominance of relatively large (~100 μm) dust grains [<xref ref-type="bibr" rid="B29">29</xref>]chemically complex molecular composition</p>
        <p>Detected species include (e.g., [<xref ref-type="bibr" rid="B30">30</xref>]-[<xref ref-type="bibr" rid="B38">38</xref>]):</p>
        <p>Optical: CN, NiRadio: CH₃OH, HCNInfrared: H<sub>2</sub>O, CO<sub>2</sub>, CO, CH<sub>4</sub></p>
        <p>Post-perihelion evolution shows:</p>
        <p>increasing CO productionemergence of organic emission bands (3.2 - 3.4 μm)asymmetry in H<sub>2</sub>O production rates</p>
        <p>A key observational result is the elevated CO<sub>2</sub>/H<sub>2</sub>O ratio, significantly above typical cometary values.</p>
        <p><bold>Key question:</bold> What is the origin of the complex chemistry and large dust grains? Within conventional models, these properties are attributed to primordial composition modified by irradiation. Within the present framework, they arise from ongoing internal processes associated with the nucleus.</p>
      </sec>
      <sec id="sec8dot4">
        <title>8.4. Sun-Facing Plume and Rotational Modulation</title>
        <p>During mid-2025, the coma exhibited a pronounced sunward-directed plume, distinct from the classical anti-solar tail [<xref ref-type="bibr" rid="B23">23</xref>]-[<xref ref-type="bibr" rid="B25">25</xref>][<xref ref-type="bibr" rid="B31">31</xref>][<xref ref-type="bibr" rid="B39">39</xref>][<xref ref-type="bibr" rid="B40">40</xref>]. This feature:</p>
        <p>originates from localized activity on the illuminated hemisphereis consistent with anisotropic emission of large dust particlesresembles behavior observed in C/2014 UN271 (Bernardinelli-Bernstein) [<xref ref-type="bibr" rid="B41">41</xref>]</p>
        <p>Subsequent observations revealed [<xref ref-type="bibr" rid="B42">42</xref>][<xref ref-type="bibr" rid="B43">43</xref>]:</p>
        <p>a persistent sunward plume linked to a localized active regiona faint high-latitude jet in the inner comaperiodic modulation of jet orientation</p>
        <p>The inferred rotation period is:</p>
        <disp-formula id="FD69">
          <mml:math>
            <mml:mrow>
              <mml:msub>
                <mml:mi>P</mml:mi>
                <mml:mrow>
                  <mml:mtext>rot</mml:mtext>
                </mml:mrow>
              </mml:msub>
              <mml:mo>=</mml:mo>
              <mml:mrow>
                <mml:mo>(</mml:mo>
                <mml:mrow>
                  <mml:mn>15.48</mml:mn>
                  <mml:mo>±</mml:mo>
                  <mml:mn>0.70</mml:mn>
                </mml:mrow>
                <mml:mo>)</mml:mo>
              </mml:mrow>
              <mml:mtext>h</mml:mtext>
            </mml:mrow>
          </mml:math>
        </disp-formula>
        <p>consistent with photometric estimates of rotation period: <inline-formula><mml:math><mml:mrow><mml:mi> T </mml:mi><mml:mo> = </mml:mo><mml:mrow><mml:mo> ( </mml:mo><mml:mrow><mml:mn> 16.16 </mml:mn><mml:mo> ± </mml:mo><mml:mn> 0.01 </mml:mn></mml:mrow><mml:mo> ) </mml:mo></mml:mrow><mml:mtext> h </mml:mtext></mml:mrow></mml:math></inline-formula> [<xref ref-type="bibr" rid="B27">27</xref>]. This represents one of the clearest detections of rotationally modulated jet activity in a cometary coma.</p>
      </sec>
      <sec id="sec8dot5">
        <title>8.5. WUC Interpretation of Observations</title>
        <p>Within the present framework, the same observational dataset admits a fundamentally different interpretation:</p>
        <p><bold>1</bold><bold>)</bold><bold>Internal Chemical Producti</bold><bold>on</bold></p>
        <p>Molecular species are generated by ongoing processes associated with UCPs, rather than being solely primordial. The observed composition reflects active internal chemistry.</p>
        <p><bold>2</bold><bold>)</bold><bold>Coma as a Self-Annihilating Reactor (SAR) Outp</bold><bold>ut</bold></p>
        <p>The coma is continuously replenished by internally generated gas and dust:</p>
        <p>no requirement for preserved “pristine” materialsustained activity independent of heliocentric distance</p>
        <p><bold>3</bold><bold>)</bold><bold>X-</bold><bold>Ray</bold><bold>Emission Mechani</bold><bold>sm</bold></p>
        <p>X-ray emission may include contributions from:</p>
        <p>gamma radiation produced by UCP self-annihilationsubsequent interaction with coma gases</p>
        <p><bold>4</bold><bold>)</bold><bold>Isotopic and Chemical Anomali</bold><bold>es</bold></p>
        <p>Observed compositional anomalies are interpreted as signatures of ongoing particle processes rather than evidence of ancient interstellar origin.</p>
        <p><bold>Synthes</bold><bold>is</bold></p>
        <p>The principal observational features of C/2025 N1 (ATLAS):</p>
        <p>strong NGAunusual chemical compositiondominance of large dust grainspersistent activity at large heliocentric distances</p>
        <p>are commonly interpreted as evidence for an interstellar origin and prolonged cosmic-ray processing.</p>
        <p>Within the present framework, these same features are instead understood as intrinsic properties of SB3 characterized by:</p>
        <p>an active UCM nucleuscontinuous matter and energy productioninternal conversion of rotational energy into translational motion</p>
        <p>This interpretation provides a unified explanation of both the dynamical and physical properties of the object without invoking an interstellar origin.</p>
      </sec>
    </sec>
    <sec id="sec9">
      <title>9. WUC Explanation of 3I/ATLAS Observations</title>
      <p>The full set of observations of C/2025 N1 (ATLAS) and related small bodies can be interpreted coherently within the present framework. In this approach, the dominant factor governing their behavior is not external forcing but internal physical processes within the nuclei and comae.</p>
      <sec id="sec9dot1">
        <title>9.1. Non-Gravitational Acceleration</title>
        <p>NGA arises from internal energy conversion and is characterized by:</p>
        <p>quasi-constant magnitudeweak dependence on heliocentric distancepersistence even at large distances where sublimation is negligible</p>
      </sec>
      <sec id="sec9dot2">
        <title>9.2. Spin Evolution of the Nucleus</title>
        <p>The rotational state of the nucleus is expected to evolve through:</p>
        <p>systematic angular momentum loss due to internal processesdiscrete, step-like changes associated with micro-volcano (MiV) eventslong-term evolution toward a critical rotation state</p>
      </sec>
      <sec id="sec9dot3">
        <title>9.3. Coma Composition and Evolution</title>
        <p>The coma is internally generated and its composition exhibits:</p>
        <p>non-solar abundance ratiostemporal variability not strictly correlated with heliocentric distanceemergence of previously undetected molecular species</p>
      </sec>
      <sec id="sec9dot4">
        <title>9.4. Dust Grain Properties</title>
        <p>Dust production is linked to Micro-world processes, leading to:</p>
        <p>characteristic grain sizes about 10<sup>2</sup> μmcontinuous replenishment independent of solar heating</p>
      </sec>
      <sec id="sec9dot5">
        <title>9.5. Sun-Facing Plume</title>
        <p>The sunward-directed plume is interpreted as a consequence of ram-pressure-driven activation. As the Small Body moves through the Interplanetary Medium, compression of the upstream gas leads to adiabatic heating. This increases the effective density within the nucleus, enhancing the efficiency of the self-annihilating reactor (SAR). As a result:</p>
        <p>internal energy release intensifiesdust production increases preferentially in the sunward directiona persistent sun-facing plume is generated</p>
      </sec>
      <sec id="sec9dot6">
        <title>9.6. Activity at Large Heliocentric Distances</title>
        <p>Sustained activity is expected at all heliocentric distances, including regions where solar-driven sublimation is negligible. Gas and dust production are therefore intrinsic rather than externally driven.</p>
      </sec>
      <sec id="sec9dot7">
        <title>9.7. X-Ray and High-Energy Signatures</title>
        <p>X-ray emission is interpreted as arising from:</p>
        <p>interaction of internally generated gamma radiation with coma gasesrather than solely from solar wind charge exchange</p>
      </sec>
      <sec id="sec9dot8">
        <title>9.8. Trajectory Evolution</title>
        <p>The trajectory is expected to show:</p>
        <p>systematic deviations from purely gravitational plus outgassing modelspersistent excess velocity not reproducible by standard non-gravitational laws</p>
      </sec>
      <sec id="sec9dot9">
        <title>9.9. Broader Population Prediction Final Statement</title>
        <p>WUC predicts that a subset of long-period comets will exhibit:</p>
        <p>anomalously high NGAunusual chemical compositionssimilar dynamical signatures indicative of internal energy processes</p>
      </sec>
      <sec id="sec9dot10">
        <title>9.10. Dark Comets and Low-Albedo Asteroids</title>
        <p>“Dark comets” and objects such as ʻOumuamua are interpreted as small bodies that:</p>
        <p>exhibit measurable NGAlack visible comae or dust tails</p>
        <p>Their dynamics are explained by the same internal mechanism—conversion of rotational energy of the nucleus into translational kinetic energy.</p>
        <p>Extremely low albedo values (0.02 - 0.08) are attributed to:</p>
        <p>low concentrations of ordinary matter in the surrounding comadominance of non-luminous Universe-Created Matter</p>
        <p><bold>Final Stateme</bold><bold>nt</bold></p>
        <p>Within the present framework, internal energy mechanisms are fundamental in governing the dynamical behavior of C/2025 N1 (ATLAS). These processes are not secondary corrections but primary drivers that determine the object’s origin, evolution, and observable properties. More broadly, they offer a new perspective on Small-Body physics and the processes underlying SS formation.</p>
      </sec>
    </sec>
    <sec id="sec10">
      <title>10. Conclusions</title>
      <p>World-Universe Cosmology provides a self-consistent framework capable of describing key cosmological parameters and their interrelations while offering quantitative predictions. In several cases, WUC yields values that align closely with observational data, strengthening its internal coherence.</p>
      <p>The model does not claim to explain all cosmological phenomena, nor to constitute a complete and final theory. Substantial further development is required. However, in its current form, WUC offers a viable foundation for a new classical cosmological framework, echoing ideas originally proposed by Dirac in 1937.</p>
      <p>The Solar System has effectively become an experimental laboratory for astrophysics, providing high-quality observational constraints. Recent advances in observational astronomy open the possibility of testing new physical models at unprecedented levels of precision.</p>
      <p>We are entering a new era in astronomy, cosmology, and astrophysics. Continued progress will depend on the willingness to explore alternative frameworks and to confront them with observational data.</p>
    </sec>
    <sec id="sec11">
      <title>Acknowledgements</title>
      <p>The author expresses deep gratitude to Alexander Prokhorov and Alexander Manenkov for their pivotal influence on his scientific development.</p>
      <p>Special acknowledgment is given to Paul Dirac, whose visionary ideas continue to inspire this work, and to Nikola Tesla for his enduring scientific legacy.</p>
      <p>The author thanks Christian Corda for publishing related manuscripts, and Robert Kuhn, Nicholas Percival, and Harry Ricker for valuable comments that improved the clarity and scope of this work.</p>
      <p>The author also expresses his deepest gratitude to his wife, Anna Netchitailo, for her unwavering support over many years.</p>
    </sec>
  </body>
  <back>
    <ref-list>
      <title>References</title>
      <ref id="B1">
        <label>1.</label>
        <citation-alternatives>
          <mixed-citation publication-type="journal">Netchitailo, V.S. (2019) High-Energy Atmospheric Physics: Ball Lightning. <italic>Journal of</italic><italic>High Energy Physics</italic>, <italic>Gravitation and Cosmology</italic>, 5, 360-374. https://doi.org/10.4236/jhepgc.2019.52020 <pub-id pub-id-type="doi">10.4236/jhepgc.2019.52020</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.4236/jhepgc.2019.52020">https://doi.org/10.4236/jhepgc.2019.52020</ext-link></mixed-citation>
          <element-citation publication-type="journal">
            <person-group person-group-type="author">
              <string-name>Netchitailo, V.S.</string-name>
              <string-name>Physics, G</string-name>
            </person-group>
            <year>2019</year>
            <article-title>High-Energy Atmospheric Physics: Ball Lightning</article-title>
            <source>Journal of High Energy Physics</source>
            <volume>5</volume>
            <pub-id pub-id-type="doi">10.4236/jhepgc.2019.52020</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B2">
        <label>2.</label>
        <citation-alternatives>
          <mixed-citation publication-type="journal">Netchitailo, V.S. (2024) Dark Galaxies, Sun-Earth-Moon Interaction, Tunguska Event-Explained by WUM. <italic>Journal of High Energy Physics</italic>, <italic>Gravitation and Cosmology</italic>, 10, 836-853. https://doi.org/10.4236/jhepgc.2024.102052 <pub-id pub-id-type="doi">10.4236/jhepgc.2024.102052</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.4236/jhepgc.2024.102052">https://doi.org/10.4236/jhepgc.2024.102052</ext-link></mixed-citation>
          <element-citation publication-type="journal">
            <person-group person-group-type="author">
              <string-name>Netchitailo, V.S.</string-name>
              <string-name>Galaxies, S</string-name>
              <string-name>Interaction, T</string-name>
              <string-name>Physics, G</string-name>
            </person-group>
            <year>2024</year>
            <article-title>Dark Galaxies, Sun-Earth-Moon Interaction, Tunguska Event-Explained by WUM</article-title>
            <source>Journal of High Energy Physics</source>
            <volume>10</volume>
            <pub-id pub-id-type="doi">10.4236/jhepgc.2024.102052</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B3">
        <label>3.</label>
        <citation-alternatives>
          <mixed-citation publication-type="other">Micheli, M., Farnocchia, D., Meech, K.J., Buie, M.W., Hainaut, O.R., Prialnik, D., <italic>et</italic><italic>al</italic>. (2018) Non-Gravitational Acceleration in the Trajectory of 1I/2017 U1 (Oumuamua). <italic>Nature</italic>, 559, 223-226. https://doi.org/10.1038/s41586-018-0254-4 <pub-id pub-id-type="doi">10.1038/s41586-018-0254-4</pub-id><pub-id pub-id-type="pmid">29950718</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.1038/s41586-018-0254-4">https://doi.org/10.1038/s41586-018-0254-4</ext-link></mixed-citation>
          <element-citation publication-type="other">
            <person-group person-group-type="author">
              <string-name>Micheli, M.</string-name>
              <string-name>Farnocchia, D.</string-name>
              <string-name>Meech, K.J.</string-name>
              <string-name>Buie, M.W.</string-name>
              <string-name>Hainaut, O.R.</string-name>
              <string-name>Prialnik, D.</string-name>
            </person-group>
            <year>2018</year>
            <article-title>Non-Gravitational Acceleration in the Trajectory of 1I/2017 U1 (Oumuamua)</article-title>
            <source>Nature</source>
            <volume>559</volume>
            <pub-id pub-id-type="doi">10.1038/s41586-018-0254-4</pub-id>
            <pub-id pub-id-type="pmid">29950718</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B4">
        <label>4.</label>
        <citation-alternatives>
          <mixed-citation publication-type="other">Eubanks, T.M., Hibberd, A., Bills, B.G., Blase, W.P., Hein, A.M., Kennedy, R.G., <italic>et al</italic>. (2025) Astrometry with Interplanetary Spacecraft: Determination of the Non-Gravitational Accelerations of the Interstellar Object 3I/ATLAS. <italic>Research Notes of the AAS</italic>, 9, 329. https://doi.org/10.3847/2515-5172/ae2915 <pub-id pub-id-type="doi">10.3847/2515-5172/ae2915</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.3847/2515-5172/ae2915">https://doi.org/10.3847/2515-5172/ae2915</ext-link></mixed-citation>
          <element-citation publication-type="other">
            <person-group person-group-type="author">
              <string-name>Eubanks, T.M.</string-name>
              <string-name>Hibberd, A.</string-name>
              <string-name>Bills, B.G.</string-name>
              <string-name>Blase, W.P.</string-name>
              <string-name>Hein, A.M.</string-name>
              <string-name>Kennedy, R.G.</string-name>
            </person-group>
            <year>2025</year>
            <article-title>Astrometry with Interplanetary Spacecraft: Determination of the Non-Gravitational Accelerations of the Interstellar Object 3I/ATLAS</article-title>
            <source>Research Notes of the AAS</source>
            <volume>9</volume>
            <pub-id pub-id-type="doi">10.3847/2515-5172/ae2915</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B5">
        <label>5.</label>
        <citation-alternatives>
          <mixed-citation publication-type="journal">Neukart, F. (2025) Non-Gravitational Acceleration in 3I ATLAS: Constraints on Exotic Volatile Outgassing in Interstellar Comets. arXiv:2511.07450.</mixed-citation>
          <element-citation publication-type="journal">
            <person-group person-group-type="author">
              <string-name>Neukart, F.</string-name>
            </person-group>
            <year>2025</year>
            <article-title>Non-Gravitational Acceleration in 3I ATLAS: Constraints on Exotic Volatile Outgassing in Interstellar Comets</article-title>
            <fpage>2511</fpage>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B6">
        <label>6.</label>
        <citation-alternatives>
          <mixed-citation publication-type="journal">Scarmato, T. (2025) Interstellar Interloper 3I/ATLAS: Nucleus Size, Photometry in RGB, Af(rho) and Antitail Structure Analysis. arXiv:2512.22365.</mixed-citation>
          <element-citation publication-type="journal">
            <person-group person-group-type="author">
              <string-name>Scarmato, T.</string-name>
              <string-name>Size, P</string-name>
              <string-name>RGB, A</string-name>
            </person-group>
            <year>2025</year>
            <article-title>Interstellar Interloper 3I/ATLAS: Nucleus Size, Photometry in RGB, Af(rho) and Antitail Structure Analysis</article-title>
            <fpage>2512</fpage>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B7">
        <label>7.</label>
        <citation-alternatives>
          <mixed-citation publication-type="other">Ahuja, G. and Ganesh, S. (2026) Effect of Different Non-Gravitational Accelerations on the Trajectory of Interstellar Comet 3I/ATLAS. <italic>Research Notes of the AAS</italic>, 10, 19. https://doi.org/10.3847/2515-5172/ae3c09 <pub-id pub-id-type="doi">10.3847/2515-5172/ae3c09</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.3847/2515-5172/ae3c09">https://doi.org/10.3847/2515-5172/ae3c09</ext-link></mixed-citation>
          <element-citation publication-type="other">
            <person-group person-group-type="author">
              <string-name>Ahuja, G.</string-name>
              <string-name>Ganesh, S.</string-name>
            </person-group>
            <year>2026</year>
            <article-title>Effect of Different Non-Gravitational Accelerations on the Trajectory of Interstellar Comet 3I/ATLAS</article-title>
            <source>Research Notes of the AAS</source>
            <volume>10</volume>
            <pub-id pub-id-type="doi">10.3847/2515-5172/ae3c09</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B8">
        <label>8.</label>
        <citation-alternatives>
          <mixed-citation publication-type="other">Spada, F., Królikowska, M. and Dones, L. (2026) Systematic and Statistical Uncertainties in the Nongravitational Acceleration of 3I/ATLAS. https://doi.org/10.1051/0004-6361/202659645 <pub-id pub-id-type="doi">10.1051/0004-6361/202659645</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.1051/0004-6361/202659645">https://doi.org/10.1051/0004-6361/202659645</ext-link></mixed-citation>
          <element-citation publication-type="other">
            <person-group person-group-type="author">
              <string-name>Spada, F.</string-name>
              <string-name>Dones, L.</string-name>
            </person-group>
            <year>2026</year>
            <article-title>Systematic and Statistical Uncertainties in the Nongravitational Acceleration of 3I/ATLAS</article-title>
            <pub-id pub-id-type="doi">10.1051/0004-6361/202659645</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B9">
        <label>9.</label>
        <citation-alternatives>
          <mixed-citation publication-type="web">Oumuamua (A/2017 U1) (2018) Small-Body Database Lookup. Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/tools/sbdb_lookup.html#/?sstr=1I%2F2017%20U1</mixed-citation>
          <element-citation publication-type="web">
            <year>2017</year>
            <article-title>(2018) Small-Body Database Lookup</article-title>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B10">
        <label>10.</label>
        <citation-alternatives>
          <mixed-citation publication-type="web">C/2019 Q4 (Borisov) (2024) Small-Body Database Lookup. Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/tools/sbdb_lookup.html#/?sstr=2I%2FBorisov</mixed-citation>
          <element-citation publication-type="web">
            <year>2019</year>
            <article-title>(2024) Small-Body Database Lookup</article-title>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B11">
        <label>11.</label>
        <citation-alternatives>
          <mixed-citation publication-type="web">C/2025 N1 (ATLAS) (2026) Small-Body Database Lookup. Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/tools/sbdb_lookup.html#/?sstr=3I%2FAtlas</mixed-citation>
          <element-citation publication-type="web">
            <year>2025</year>
            <article-title>(2026) Small-Body Database Lookup</article-title>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B12">
        <label>12.</label>
        <citation-alternatives>
          <mixed-citation publication-type="web">Oreshko, A.G. (2012) Observation of Dark Spherical Area after Passage of Ball Lightning through Thick Absorbers. https://www.researchgate.net/profile/Alexander_Oreshko/publication/312218738_Observation_of_Dark_Spherical_Area_After_Passage_of_Ball_Lightning_Through_Thick_Absorbers/links/5877307808ae329d6226e786/Observation-of-Dark-Spherical-Area-After-Passage-of-Ball-Lightning-Through-Thick-Absorbers.pdf</mixed-citation>
          <element-citation publication-type="web">
            <person-group person-group-type="author">
              <string-name>Oreshko, A.G.</string-name>
            </person-group>
            <year>2012</year>
            <article-title>Observation of Dark Spherical Area after Passage of Ball Lightning through Thick Absorbers</article-title>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B13">
        <label>13.</label>
        <citation-alternatives>
          <mixed-citation publication-type="web">Wolfenstein, L. (1994) Superweak Interactions. https://cds.cern.ch/record/264313/files/P00023830.pdf</mixed-citation>
          <element-citation publication-type="web">
            <person-group person-group-type="author">
              <string-name>Wolfenstein, L.</string-name>
            </person-group>
            <year>1994</year>
            <article-title>Superweak Interactions</article-title>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B14">
        <label>14.</label>
        <citation-alternatives>
          <mixed-citation publication-type="journal">Netchitailo, V.S. (2024) Cosmic Bubbles. <italic>Journal of High Energy Physics</italic>, <italic>Gravitation and Cosmology</italic>, 10, 438-453. https://doi.org/10.4236/jhepgc.2024.101029 <pub-id pub-id-type="doi">10.4236/jhepgc.2024.101029</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.4236/jhepgc.2024.101029">https://doi.org/10.4236/jhepgc.2024.101029</ext-link></mixed-citation>
          <element-citation publication-type="journal">
            <person-group person-group-type="author">
              <string-name>Netchitailo, V.S.</string-name>
              <string-name>Physics, G</string-name>
            </person-group>
            <year>2024</year>
            <article-title>Cosmic Bubbles</article-title>
            <source>Journal of High Energy Physics</source>
            <volume>10</volume>
            <pub-id pub-id-type="doi">10.4236/jhepgc.2024.101029</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B15">
        <label>15.</label>
        <citation-alternatives>
          <mixed-citation publication-type="journal">Ren, X., Yan, W., Zhao, R.N., Wang, S., <italic>et al</italic>. (2026) Interstellar Object 3I/ATLAS Observed from Mars by China’s Tianwen-1 Spacecraft. arXiv:2603.10350. https://doi.org/10.3847/2041-8213/ae61b3 <pub-id pub-id-type="doi">10.3847/2041-8213/ae61b3</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.3847/2041-8213/ae61b3">https://doi.org/10.3847/2041-8213/ae61b3</ext-link></mixed-citation>
          <element-citation publication-type="journal">
            <person-group person-group-type="author">
              <string-name>Ren, X.</string-name>
              <string-name>Yan, W.</string-name>
              <string-name>Zhao, R.N.</string-name>
              <string-name>Wang, S.</string-name>
            </person-group>
            <year>2026</year>
            <article-title>Interstellar Object 3I/ATLAS Observed from Mars by China’s Tianwen-1 Spacecraft</article-title>
            <fpage>2603</fpage>
            <pub-id pub-id-type="doi">10.3847/2041-8213/ae61b3</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B16">
        <label>16.</label>
        <citation-alternatives>
          <mixed-citation publication-type="web">3I/ATLAS (2026) 3I/ATLAS. Wikipedia. https://en.wikipedia.org/wiki/3I/ATLAS</mixed-citation>
          <element-citation publication-type="web">
            <year>2026</year>
            <article-title>3I/ATLAS</article-title>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B17">
        <label>17.</label>
        <citation-alternatives>
          <mixed-citation publication-type="journal">Belyakov, M., Wong, I., Bolin, B.T., Davis, M.R., Bromley, S.J., Lisse, C.M., <italic>et al</italic>. (2026) The Volatile Inventory of 3I/ATLAS as Seen with JWST/MIRI. <italic>The Astrophysical Journal Letters</italic>, 1001, L11. https://doi.org/10.3847/2041-8213/ae5700 <pub-id pub-id-type="doi">10.3847/2041-8213/ae5700</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.3847/2041-8213/ae5700">https://doi.org/10.3847/2041-8213/ae5700</ext-link></mixed-citation>
          <element-citation publication-type="journal">
            <person-group person-group-type="author">
              <string-name>Belyakov, M.</string-name>
              <string-name>Wong, I.</string-name>
              <string-name>Bolin, B.T.</string-name>
              <string-name>Davis, M.R.</string-name>
              <string-name>Bromley, S.J.</string-name>
              <string-name>Lisse, C.M.</string-name>
            </person-group>
            <year>2026</year>
            <article-title>The Volatile Inventory of 3I/ATLAS as Seen with JWST/MIRI</article-title>
            <source>The Astrophysical Journal Letters</source>
            <volume>1001</volume>
            <pub-id pub-id-type="doi">10.3847/2041-8213/ae5700</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B18">
        <label>18.</label>
        <citation-alternatives>
          <mixed-citation publication-type="web">The European Space Agency (2026) First Glimpse of Comet 3I/ATLAS from Juice Science Camera. https://www.esa.int/ESA_Multimedia/Images/2026/02/First_glimpse_of_comet_3I_ATLAS_from_Juice_science_camera</mixed-citation>
          <element-citation publication-type="web">
            <year>2026</year>
            <article-title>First Glimpse of Comet 3I/ATLAS from Juice Science Camera</article-title>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B19">
        <label>19.</label>
        <citation-alternatives>
          <mixed-citation publication-type="web">SETI Institute (2026) 3I/ATLAS: Caught in UV What Europa Clipper Saw When No One Else Could. https://www.seti.org/news/3iatlas-caught-in-uv-what-europa-clipper-saw-when-no-one-else-could/#:~:text=Before%20this%20observation%2C%20it%20was,structures%20rather%20than%20transient%20artifacts</mixed-citation>
          <element-citation publication-type="web">
            <year>2026</year>
            <article-title>3I/ATLAS: Caught in UV What Europa Clipper Saw When No One Else Could</article-title>
            <source>https://www.seti.org/news/3iatlas-caught-in-uv-what-europa-clipper-saw-when-no-one-else-could/#:~:text=Before%20this%20observation%2C%20it%20was</source>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B20">
        <label>20.</label>
        <citation-alternatives>
          <mixed-citation publication-type="web">News Staff (2025) XMM-Newton Offers Incredible X-Ray View of Interstellar Comet 3I/ATLAS. https://www.sci.news/astronomy/xmm-newton-x-ray-view-interstellar-comet-3i-atlas-14420.html#:~:text=Astronomers%20using%20ESA’s%20XMM%2DNewton,team%20said%20in%20a%20statement</mixed-citation>
          <element-citation publication-type="web">
            <year>2025</year>
            <article-title>XMM-Newton Offers Incredible X-Ray View of Interstellar Comet 3I/ATLAS</article-title>
            <source>https://www.sci.news/astronomy/xmm-newton-x-ray-view-interstellar-comet-3i-atlas-14420.html#:~:text=Astronomers%20using%20ESA’s%20XMM%2DNewton</source>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B21">
        <label>21.</label>
        <citation-alternatives>
          <mixed-citation publication-type="web">Mathewson, S. (2025) Scientists Detect X-Ray Glow from Interstellar Comet 3I/ATLAS Extending 250,000 Miles into Space. SPACE. https://www.space.com/astronomy/comets/scientists-detect-x-ray-glow-from-interstellar-comet-3i-atlas-extending-250-000-out-miles-into-space</mixed-citation>
          <element-citation publication-type="web">
            <person-group person-group-type="author">
              <string-name>Mathewson, S.</string-name>
            </person-group>
            <year>2025</year>
            <article-title>Scientists Detect X-Ray Glow from Interstellar Comet 3I/ATLAS Extending 250,000 Miles into Space</article-title>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B22">
        <label>22.</label>
        <citation-alternatives>
          <mixed-citation publication-type="web">Ishi, D., Kanemaru, Y., Fukushima, K., Ogawa, S., <italic>et al</italic>. (2025) X-Ray Observation of the Cometary Interloper C/2025 N1 (3I/ATLAS) by XRISM/Xtend. The Astronomer’s Telegram. https://www.astronomerstelegram.org/?read=17523</mixed-citation>
          <element-citation publication-type="web">
            <person-group person-group-type="author">
              <string-name>Ishi, D.</string-name>
              <string-name>Kanemaru, Y.</string-name>
              <string-name>Fukushima, K.</string-name>
              <string-name>Ogawa, S.</string-name>
            </person-group>
            <year>2025</year>
            <article-title>X-Ray Observation of the Cometary Interloper C/2025 N1 (3I/ATLAS) by XRISM/Xtend</article-title>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B23">
        <label>23.</label>
        <citation-alternatives>
          <mixed-citation publication-type="journal">Maggiolo, R., Dhooghe, F., Gronoff, G.P., de Keyser, J. and Cessateur, G. (2026) Interstellar Comet 3I/ATLAS: Evidence for Galactic Cosmic-Ray Processing. <italic>The Astrophysical Journal Letters</italic>, 996, L34. https://doi.org/10.3847/2041-8213/ae2fff <pub-id pub-id-type="doi">10.3847/2041-8213/ae2fff</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.3847/2041-8213/ae2fff">https://doi.org/10.3847/2041-8213/ae2fff</ext-link></mixed-citation>
          <element-citation publication-type="journal">
            <person-group person-group-type="author">
              <string-name>Maggiolo, R.</string-name>
              <string-name>Dhooghe, F.</string-name>
              <string-name>Gronoff, G.P.</string-name>
              <string-name>Keyser, J.</string-name>
              <string-name>Cessateur, G.</string-name>
            </person-group>
            <year>2026</year>
            <article-title>Interstellar Comet 3I/ATLAS: Evidence for Galactic Cosmic-Ray Processing</article-title>
            <source>The Astrophysical Journal Letters</source>
            <volume>996</volume>
            <pub-id pub-id-type="doi">10.3847/2041-8213/ae2fff</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B24">
        <label>24.</label>
        <citation-alternatives>
          <mixed-citation publication-type="journal">Harrington Pinto, O., Womack, M., Fernandez, Y. and Bauer, J. (2022) A Survey of CO, CO <sub>2</sub>, and H <sub>2</sub>O in Comets and Centaurs. <italic>The Planetary Science Journal</italic>, 3, 247. https://doi.org/10.3847/psj/ac960d <pub-id pub-id-type="doi">10.3847/psj/ac960d</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.3847/psj/ac960d">https://doi.org/10.3847/psj/ac960d</ext-link></mixed-citation>
          <element-citation publication-type="journal">
            <person-group person-group-type="author">
              <string-name>Pinto, O.</string-name>
              <string-name>Womack, M.</string-name>
              <string-name>Fernandez, Y.</string-name>
              <string-name>Bauer, J.</string-name>
              <string-name>CO, C</string-name>
            </person-group>
            <year>2022</year>
            <article-title>A Survey of CO, CO2, and H2O in Comets and Centaurs</article-title>
            <source>The Planetary Science Journal</source>
            <volume>3</volume>
            <pub-id pub-id-type="doi">10.3847/psj/ac960d</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B25">
        <label>25.</label>
        <citation-alternatives>
          <mixed-citation publication-type="other">Bolin, B.T., Belyakov, M., Fremling, C., Graham, M.J., Abdelaziz, A.M., Elhosseiny, E., <italic>et al</italic>. (2025) Interstellar Comet 3I/ATLAS: Discovery and Physical Description. <italic>Monthly Notices of the Royal Astronomical Society</italic>: <italic>Letters</italic>, 542, L139-L143. https://doi.org/10.1093/mnrasl/slaf078 <pub-id pub-id-type="doi">10.1093/mnrasl/slaf078</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.1093/mnrasl/slaf078">https://doi.org/10.1093/mnrasl/slaf078</ext-link></mixed-citation>
          <element-citation publication-type="other">
            <person-group person-group-type="author">
              <string-name>Bolin, B.T.</string-name>
              <string-name>Belyakov, M.</string-name>
              <string-name>Fremling, C.</string-name>
              <string-name>Graham, M.J.</string-name>
              <string-name>Abdelaziz, A.M.</string-name>
              <string-name>Elhosseiny, E.</string-name>
            </person-group>
            <year>2025</year>
            <article-title>Interstellar Comet 3I/ATLAS: Discovery and Physical Description</article-title>
            <source>Monthly Notices of the Royal Astronomical Society: Letters</source>
            <volume>542</volume>
            <pub-id pub-id-type="doi">10.1093/mnrasl/slaf078</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B26">
        <label>26.</label>
        <citation-alternatives>
          <mixed-citation publication-type="journal">Chandler, C.O., Bernardinelli, P.H., Jurić, M., <italic>et al</italic>. (2025) NSF-DOE Vera C. Rubin Observatory Observations of Interstellar Comet 3I/ATLAS (C/2025 N1). arXiv:2507.13409.</mixed-citation>
          <element-citation publication-type="journal">
            <person-group person-group-type="author">
              <string-name>Chandler, C.O.</string-name>
              <string-name>Bernardinelli, P.H.</string-name>
            </person-group>
            <year>2025</year>
            <article-title>NSF-DOE Vera C</article-title>
            <fpage>2507</fpage>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B27">
        <label>27.</label>
        <citation-alternatives>
          <mixed-citation publication-type="other">Santana-Ros, T., Ivanova, O., Mykhailova, S., Erasmus, N., Kamiński, K., Oszkiewicz, D., <italic>et al</italic>. (2025) Temporal Evolution of the Third Interstellar Comet 3I/ATLAS: Spin, Color, Spectra, and Dust Activity. <italic>Astronomy &amp; Astrophysics</italic>, 702, L3. https://doi.org/10.1051/0004-6361/202556717 <pub-id pub-id-type="doi">10.1051/0004-6361/202556717</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.1051/0004-6361/202556717">https://doi.org/10.1051/0004-6361/202556717</ext-link></mixed-citation>
          <element-citation publication-type="other">
            <person-group person-group-type="author">
              <string-name>Santana-Ros, T.</string-name>
              <string-name>Ivanova, O.</string-name>
              <string-name>Mykhailova, S.</string-name>
              <string-name>Erasmus, N.</string-name>
              <string-name>Oszkiewicz, D.</string-name>
              <string-name>Spin, C</string-name>
            </person-group>
            <year>2025</year>
            <article-title>Temporal Evolution of the Third Interstellar Comet 3I/ATLAS: Spin, Color, Spectra, and Dust Activity</article-title>
            <source>Astronomy &amp; Astrophysics</source>
            <volume>702</volume>
            <pub-id pub-id-type="doi">10.1051/0004-6361/202556717</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B28">
        <label>28.</label>
        <citation-alternatives>
          <mixed-citation publication-type="journal">Seligman, D.Z., Micheli, M., Farnocchia, D., Denneau, L., Noonan, J.W., Hsieh, H.H., <italic>et al</italic>. (2025) Discovery and Preliminary Characterization of a Third Interstellar Object: 3I/ATLAS. <italic>The Astrophysical Journal Letters</italic>, 989, L36. https://doi.org/10.3847/2041-8213/adf49a <pub-id pub-id-type="doi">10.3847/2041-8213/adf49a</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.3847/2041-8213/adf49a">https://doi.org/10.3847/2041-8213/adf49a</ext-link></mixed-citation>
          <element-citation publication-type="journal">
            <person-group person-group-type="author">
              <string-name>Seligman, D.Z.</string-name>
              <string-name>Micheli, M.</string-name>
              <string-name>Farnocchia, D.</string-name>
              <string-name>Denneau, L.</string-name>
              <string-name>Noonan, J.W.</string-name>
              <string-name>Hsieh, H.H.</string-name>
            </person-group>
            <year>2025</year>
            <article-title>Discovery and Preliminary Characterization of a Third Interstellar Object: 3I/ATLAS</article-title>
            <source>The Astrophysical Journal Letters</source>
            <volume>989</volume>
            <fpage>3</fpage>
            <pub-id pub-id-type="doi">10.3847/2041-8213/adf49a</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B29">
        <label>29.</label>
        <citation-alternatives>
          <mixed-citation publication-type="journal">Jewitt, D. and Luu, J. (2025) Preperihelion Development of Interstellar Comet 3I/ATLAS. <italic>The Astrophysical Journal Letters</italic>, 994, L3. https://doi.org/10.3847/2041-8213/ae1832 <pub-id pub-id-type="doi">10.3847/2041-8213/ae1832</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.3847/2041-8213/ae1832">https://doi.org/10.3847/2041-8213/ae1832</ext-link></mixed-citation>
          <element-citation publication-type="journal">
            <person-group person-group-type="author">
              <string-name>Jewitt, D.</string-name>
              <string-name>Luu, J.</string-name>
            </person-group>
            <year>2025</year>
            <article-title>Preperihelion Development of Interstellar Comet 3I/ATLAS</article-title>
            <source>The Astrophysical Journal Letters</source>
            <volume>994</volume>
            <pub-id pub-id-type="doi">10.3847/2041-8213/ae1832</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B30">
        <label>30.</label>
        <citation-alternatives>
          <mixed-citation publication-type="journal">Hoogendam, W.B., Shappee, B.J., Wray, J.J., <italic>et al</italic>. (2025) Spatial Profiles of 3I/ATLAS CN and Ni Outgassing from Keck/KCWI Integral Field Spectroscopy. arXiv:2510.11779.</mixed-citation>
          <element-citation publication-type="journal">
            <person-group person-group-type="author">
              <string-name>Hoogendam, W.B.</string-name>
              <string-name>Shappee, B.J.</string-name>
              <string-name>Wray, J.J.</string-name>
            </person-group>
            <year>2025</year>
            <article-title>Spatial Profiles of 3I/ATLAS CN and Ni Outgassing from Keck/KCWI Integral Field Spectroscopy</article-title>
            <fpage>2510</fpage>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B31">
        <label>31.</label>
        <citation-alternatives>
          <mixed-citation publication-type="journal">Rahatgaonkar, R., Carvajal, J.P., Puzia, T.H., Luco, B., Jehin, E., Hutsemékers, D., <italic>et</italic><italic>al</italic>. (2025) Very Large Telescope Observations of Interstellar Comet 3I/ATLAS. II. from Quiescence to Glow: Dramatic Rise of Ni I Emission and Incipient CN Outgassing at Large Heliocentric Distances. <italic>The Astrophysical Journal Letters</italic>, 995, L34. https://doi.org/10.3847/2041-8213/ae1cbc <pub-id pub-id-type="doi">10.3847/2041-8213/ae1cbc</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.3847/2041-8213/ae1cbc">https://doi.org/10.3847/2041-8213/ae1cbc</ext-link></mixed-citation>
          <element-citation publication-type="journal">
            <person-group person-group-type="author">
              <string-name>Rahatgaonkar, R.</string-name>
              <string-name>Carvajal, J.P.</string-name>
              <string-name>Puzia, T.H.</string-name>
              <string-name>Luco, B.</string-name>
              <string-name>Jehin, E.</string-name>
            </person-group>
            <year>2025</year>
            <article-title>Very Large Telescope Observations of Interstellar Comet 3I/ATLAS</article-title>
            <source>II. from Quiescence to Glow: Dramatic Rise of Ni I Emission and Incipient CN Outgassing at Large Heliocentric Distances. The Astrophysical Journal Letters</source>
            <volume>995</volume>
            <pub-id pub-id-type="doi">10.3847/2041-8213/ae1cbc</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B32">
        <label>32.</label>
        <citation-alternatives>
          <mixed-citation publication-type="journal">Manzano, L.E.S., Lin, H.W., Taylor, A.G., <italic>et al</italic>. (2025) Onset of CN Emission in 3I/ATLAS: Evidence for Strong Carbon-Chain Depletion. arXiv:2509.01647.</mixed-citation>
          <element-citation publication-type="journal">
            <person-group person-group-type="author">
              <string-name>Manzano, L.E.S.</string-name>
              <string-name>Lin, H.W.</string-name>
              <string-name>Taylor, A.G.</string-name>
            </person-group>
            <year>2025</year>
            <article-title>Onset of CN Emission in 3I/ATLAS: Evidence for Strong Carbon-Chain Depletion</article-title>
            <fpage>2509</fpage>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B33">
        <label>33.</label>
        <citation-alternatives>
          <mixed-citation publication-type="journal">Roth, N.X., Cordiner, M.A., Bockelée-Morvan, D., Biver, N., Crovisier, J., Milam, S.N., <italic>et al</italic>. (2025) CH <sub>3</sub>OH and HCN in Interstellar Comet 3I/ATLAS Mapped with the ALMA Atacama Compact Array: Distinct Outgassing Behaviors and a Remarkably High CH <sub>3</sub>OH/HCN Production Rate Ratio. <italic>The Astrophysical Journal Letters</italic>, 999, L32. https://doi.org/10.3847/2041-8213/ae433b <pub-id pub-id-type="doi">10.3847/2041-8213/ae433b</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.3847/2041-8213/ae433b">https://doi.org/10.3847/2041-8213/ae433b</ext-link></mixed-citation>
          <element-citation publication-type="journal">
            <person-group person-group-type="author">
              <string-name>Roth, N.X.</string-name>
              <string-name>Cordiner, M.A.</string-name>
              <string-name>Morvan, D.</string-name>
              <string-name>Biver, N.</string-name>
              <string-name>Crovisier, J.</string-name>
              <string-name>Milam, S.N.</string-name>
            </person-group>
            <year>2025</year>
            <article-title>CH3OH and HCN in Interstellar Comet 3I/ATLAS Mapped with the ALMA Atacama Compact Array: Distinct Outgassing Behaviors and a Remarkably High CH3OH/HCN Production Rate Ratio</article-title>
            <source>The Astrophysical Journal Letters</source>
            <volume>999</volume>
            <pub-id pub-id-type="doi">10.3847/2041-8213/ae433b</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B34">
        <label>34.</label>
        <citation-alternatives>
          <mixed-citation publication-type="other">Cordiner, M., Roth, N.X., Micheli, M., Villanueva, G., Farnocchia, D., Charnley, S., <italic>et al</italic>. (2025) Isotopic Evidence for a Cold and Distant Origin of 3I/ATLAs. <italic>Nature</italic>, 655, 870-874. https://doi.org/10.1038/s41586-026-10771-6 <pub-id pub-id-type="doi">10.1038/s41586-026-10771-6</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.1038/s41586-026-10771-6">https://doi.org/10.1038/s41586-026-10771-6</ext-link></mixed-citation>
          <element-citation publication-type="other">
            <person-group person-group-type="author">
              <string-name>Cordiner, M.</string-name>
              <string-name>Roth, N.X.</string-name>
              <string-name>Micheli, M.</string-name>
              <string-name>Villanueva, G.</string-name>
              <string-name>Farnocchia, D.</string-name>
              <string-name>Charnley, S.</string-name>
            </person-group>
            <year>2025</year>
            <article-title>Isotopic Evidence for a Cold and Distant Origin of 3I/ATLAs</article-title>
            <source>Nature</source>
            <volume>655</volume>
            <pub-id pub-id-type="doi">10.1038/s41586-026-10771-6</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B35">
        <label>35.</label>
        <citation-alternatives>
          <mixed-citation publication-type="journal">Lisse, C.M., Bach, Y.P., Crill, B.P., Korngut, P.M., <italic>et al</italic>. (2025) SPHEREx Pre-Perihelion Mapping of H <sub>2</sub>O, CO <sub>2</sub>, and CO in Interstellar Object 3I/ATLAS. arXiv:2512.07318.</mixed-citation>
          <element-citation publication-type="journal">
            <person-group person-group-type="author">
              <string-name>Lisse, C.M.</string-name>
              <string-name>Bach, Y.P.</string-name>
              <string-name>Crill, B.P.</string-name>
              <string-name>Korngut, P.M.</string-name>
            </person-group>
            <year>2025</year>
            <article-title>SPHEREx Pre-Perihelion Mapping of H2O, CO2, and CO in Interstellar Object 3I/ATLAS</article-title>
            <fpage>2512</fpage>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B36">
        <label>36.</label>
        <citation-alternatives>
          <mixed-citation publication-type="other">Lisse, C.M., Bach, Y.P., Bryan, S.A., Korngut, P.M., Crill, B.P., Cukierman, A.J., <italic>et al</italic>. (2026) SPHEREx Reobservation of Interstellar Object 3I/ATLAS in 2025 December: Detection of Increased Post-Perihelion Activity, Refractory Coma Dust, and New Coma Gas Species. <italic>Research Notes of the AAS</italic>, 10, 26. https://doi.org/10.3847/2515-5172/ae3f95 <pub-id pub-id-type="doi">10.3847/2515-5172/ae3f95</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.3847/2515-5172/ae3f95">https://doi.org/10.3847/2515-5172/ae3f95</ext-link></mixed-citation>
          <element-citation publication-type="other">
            <person-group person-group-type="author">
              <string-name>Lisse, C.M.</string-name>
              <string-name>Bach, Y.P.</string-name>
              <string-name>Bryan, S.A.</string-name>
              <string-name>Korngut, P.M.</string-name>
              <string-name>Crill, B.P.</string-name>
              <string-name>Cukierman, A.J.</string-name>
              <string-name>Activity, R</string-name>
            </person-group>
            <year>2026</year>
            <article-title>SPHEREx Reobservation of Interstellar Object 3I/ATLAS in 2025 December: Detection of Increased Post-Perihelion Activity, Refractory Coma Dust, and New Coma Gas Species</article-title>
            <source>Research Notes of the AAS</source>
            <volume>10</volume>
            <pub-id pub-id-type="doi">10.3847/2515-5172/ae3f95</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B37">
        <label>37.</label>
        <citation-alternatives>
          <mixed-citation publication-type="other">Zhang, Q. and Battams, K. (2025) Rapid Brightening of 3I/ATLAS Ahead of Perihelion. <italic>Publications of the Astronomical Society of the Pacific</italic>, 138, Article 014403. https://doi.org/10.1088/1538-3873/ae2e88 <pub-id pub-id-type="doi">10.1088/1538-3873/ae2e88</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.1088/1538-3873/ae2e88">https://doi.org/10.1088/1538-3873/ae2e88</ext-link></mixed-citation>
          <element-citation publication-type="other">
            <person-group person-group-type="author">
              <string-name>Zhang, Q.</string-name>
              <string-name>Battams, K.</string-name>
            </person-group>
            <year>2025</year>
            <article-title>Rapid Brightening of 3I/ATLAS Ahead of Perihelion</article-title>
            <source>Publications of the Astronomical Society of the Pacific</source>
            <volume>138</volume>
            <elocation-id>014403</elocation-id>
            <pub-id pub-id-type="doi">10.1088/1538-3873/ae2e88</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B38">
        <label>38.</label>
        <citation-alternatives>
          <mixed-citation publication-type="journal">Tan, H., Yan, X. and Li, J. (2026) Perihelion Asymmetry in the Water Production Rate of the Interstellar Object 3I/ATLAS. <italic>The Astrophysical Journal Letters</italic>, 998, L22. https://doi.org/10.3847/2041-8213/ae3c97 <pub-id pub-id-type="doi">10.3847/2041-8213/ae3c97</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.3847/2041-8213/ae3c97">https://doi.org/10.3847/2041-8213/ae3c97</ext-link></mixed-citation>
          <element-citation publication-type="journal">
            <person-group person-group-type="author">
              <string-name>Tan, H.</string-name>
              <string-name>Yan, X.</string-name>
              <string-name>Li, J.</string-name>
            </person-group>
            <year>2026</year>
            <article-title>Perihelion Asymmetry in the Water Production Rate of the Interstellar Object 3I/ATLAS</article-title>
            <source>The Astrophysical Journal Letters</source>
            <volume>998</volume>
            <pub-id pub-id-type="doi">10.3847/2041-8213/ae3c97</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B39">
        <label>39.</label>
        <citation-alternatives>
          <mixed-citation publication-type="journal">Jewitt, D., Hui, M., Mutchler, M., Kim, Y. and Agarwal, J. (2025) Hubble Space Telescope Observations of the Interstellar Interloper 3I/ATLAS. <italic>The Astrophysical Journal Letters</italic>, 990, L2. https://doi.org/10.3847/2041-8213/adf8d8 <pub-id pub-id-type="doi">10.3847/2041-8213/adf8d8</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.3847/2041-8213/adf8d8">https://doi.org/10.3847/2041-8213/adf8d8</ext-link></mixed-citation>
          <element-citation publication-type="journal">
            <person-group person-group-type="author">
              <string-name>Jewitt, D.</string-name>
              <string-name>Hui, M.</string-name>
              <string-name>Mutchler, M.</string-name>
              <string-name>Kim, Y.</string-name>
              <string-name>Agarwal, J.</string-name>
            </person-group>
            <year>2025</year>
            <article-title>Hubble Space Telescope Observations of the Interstellar Interloper 3I/ATLAS</article-title>
            <source>The Astrophysical Journal Letters</source>
            <volume>990</volume>
            <pub-id pub-id-type="doi">10.3847/2041-8213/adf8d8</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B40">
        <label>40.</label>
        <citation-alternatives>
          <mixed-citation publication-type="journal">Tonry, J.L., Denneau, L., Alarcón, M.R., Clocchiatti, A., Erasmus, N., Fitzsimmons, A., <italic>et al</italic>. (2025) ATLAS Photometry of Interstellar Object 3I/ATLAS. <italic>The Astrophysical Journal Letters</italic>, 995, L15. https://doi.org/10.3847/2041-8213/ae1f12 <pub-id pub-id-type="doi">10.3847/2041-8213/ae1f12</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.3847/2041-8213/ae1f12">https://doi.org/10.3847/2041-8213/ae1f12</ext-link></mixed-citation>
          <element-citation publication-type="journal">
            <person-group person-group-type="author">
              <string-name>Tonry, J.L.</string-name>
              <string-name>Denneau, L.</string-name>
              <string-name>Clocchiatti, A.</string-name>
              <string-name>Erasmus, N.</string-name>
              <string-name>Fitzsimmons, A.</string-name>
            </person-group>
            <year>2025</year>
            <article-title>ATLAS Photometry of Interstellar Object 3I/ATLAS</article-title>
            <source>The Astrophysical Journal Letters</source>
            <volume>995</volume>
            <pub-id pub-id-type="doi">10.3847/2041-8213/ae1f12</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B41">
        <label>41.</label>
        <citation-alternatives>
          <mixed-citation publication-type="journal">Sekanina, Z. (1974) On the Nature of the Anti-Tail of Comet Kohoutek (1973f) I. A Working Model. <italic>Icarus</italic>, 23, 502-518. https://doi.org/10.1016/0019-1035(74)90013-x <pub-id pub-id-type="doi">10.1016/0019-1035(74)90013-x</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.1016/0019-1035(74)90013-x">https://doi.org/10.1016/0019-1035(74)90013-x</ext-link></mixed-citation>
          <element-citation publication-type="journal">
            <person-group person-group-type="author">
              <string-name>Sekanina, Z.</string-name>
            </person-group>
            <year>1974</year>
            <article-title>On the Nature of the Anti-Tail of Comet Kohoutek (1973f) I</article-title>
            <source>A Working Model. Icarus</source>
            <volume>1035</volume>
            <issue>74</issue>
            <pub-id pub-id-type="doi">10.1016/0019-1035(74)90013-x</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B42">
        <label>42.</label>
        <citation-alternatives>
          <mixed-citation publication-type="other">Serra-Ricart, M., Licandro, J. and Alarcon, M.R. (2026) Pre-Perihelion Detection of a Wobbling High-Latitude Jet in the Interstellar Comet 3I/ATLAS. <italic>Astronomy &amp; Astrophysics</italic>, 705, L3. https://doi.org/10.1051/0004-6361/202558072 <pub-id pub-id-type="doi">10.1051/0004-6361/202558072</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.1051/0004-6361/202558072">https://doi.org/10.1051/0004-6361/202558072</ext-link></mixed-citation>
          <element-citation publication-type="other">
            <person-group person-group-type="author">
              <string-name>Serra-Ricart, M.</string-name>
              <string-name>Licandro, J.</string-name>
              <string-name>Alarcon, M.R.</string-name>
            </person-group>
            <year>2026</year>
            <article-title>Pre-Perihelion Detection of a Wobbling High-Latitude Jet in the Interstellar Comet 3I/ATLAS</article-title>
            <source>Astronomy &amp; Astrophysics</source>
            <volume>705</volume>
            <pub-id pub-id-type="doi">10.1051/0004-6361/202558072</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
      <ref id="B43">
        <label>43.</label>
        <citation-alternatives>
          <mixed-citation publication-type="journal">Sekanina, Z. and Miller, F.D. (1976) On the Nature of the Anti-Tail of Comet Kohoutek (1973f). II. Comparison of the Working Model with Ground-Based Photographic Observations. <italic>Icarus</italic>, 27, 135-146. https://doi.org/10.1016/0019-1035(76)90190-1 <pub-id pub-id-type="doi">10.1016/0019-1035(76)90190-1</pub-id><ext-link ext-link-type="uri" xlink:href="https://doi.org/10.1016/0019-1035(76)90190-1">https://doi.org/10.1016/0019-1035(76)90190-1</ext-link></mixed-citation>
          <element-citation publication-type="journal">
            <person-group person-group-type="author">
              <string-name>Sekanina, Z.</string-name>
              <string-name>Miller, F.D.</string-name>
            </person-group>
            <year>1976</year>
            <article-title>On the Nature of the Anti-Tail of Comet Kohoutek (1973f)</article-title>
            <source>II. Comparison of the Working Model with Ground-Based Photographic Observations. Icarus</source>
            <volume>1035</volume>
            <issue>76</issue>
            <pub-id pub-id-type="doi">10.1016/0019-1035(76)90190-1</pub-id>
          </element-citation>
        </citation-alternatives>
      </ref>
    </ref-list>
  </back>
</article>