ijaa International Journal of Astronomy and Astrophysics 2161-4725 2161-4717 Scientific Research Publishing 10.4236/ijaa.2023.131001 ijaa-123758 Article Physics Mathematics Transport in Astrophysics: III. Diffusion from the Galactic Plane Zaninetti Lorenzo 1 Physics Department, University of Turin, Turin, Italy

The author declares no conflicts of interest regarding the publication of this paper.

 17 03 2023 03 2023 13 01 1 24 21 12 2022 17 03 2023 20 03 2023 © 2023 by the authors and Scientific Research Publishing Inc. 2023 This article is an open access article distributed under the terms and conditions of the Creative Commons Attribution (CC BY) license ( https://creativecommons.org/licenses/by/4.0/ ). https://doi.org/10.4236/ijaa.2023.131001

New solutions, for the stationary and temporary states, are derived for the 1D diffusion of cosmic rays in the presence of losses. The new results are applied to the latitude profile of radiation emitted above the galactic plane. Percolation theory for a spiral galaxy coupled with the evolution of the super-bubbles allows building a model for the radiation of a spiral galaxy as seen face on. The annulus of radiation of our galaxy is also simulated and the excess of radiation observed at the centre of our galaxy is explained by the sine law which arises in the theory of the image.

 Particle Diffusion Galaxy: Centre Galaxy: Disk 1. Introduction

We now analyse, in chronological order, some topics raised by the connection between the acceleration/diffusion/confinement of cosmic rays (CR) and superbubbles/super-shells (SB): the CR confinement from SBs means that the mean age would be independent of energy [1], the constancy of CR-produced Be relative to supernova-produced Fe observed in halo stars formed in the early Galaxy [2], a model for the observations of the evolution of 6LiBeB [3], an explanation for the well-known anomalous 22Ne/20Ne ratio [4], the acceleration of cosmic-ray nuclei heavier than He in enriched SB interiors [5], production of CR by suprathermal ion injection [6], a discussion of the fraction of the unaccounted for energy which is converted in CR [7], an investigation of the shape of the spectrum of high-energy protons produced inside the SB blown around clusters of massive stars [8], a model based on two coupled stochastic differential equations, which is applied to protons and alpha particles [9], a discussion of the non-thermal spectrum between 1.5 and 8.8 GHz which is fitted with a standard model of an aging cosmic-ray electron population [10], a model which includes advection, diffusion, thermal conduction and radiative cooling for CR [11], a framework tying together the sources, injection, acceleration, and propagation of CRs [12], an evaluation of the distribution of pions from continuous losses of CR [13], analysis of the generalized Kompaneets’ equations adapted to expansion in various external density profiles and coupled with escaping CRs [14], production of γ-ray radiation in the interactions between cosmic rays and interstellar gas in the Orion-Eridanus SB [15] and acceleration of particles and non-linear feedback [16]. Another point for research is the excess in γ-rays observed by the Fermi Large Area Telescope at the centre of the Galaxy, which can be explained by annihilating dark matter, [17]. The already cited papers leave a series of questions unanswered or only partially answered:

Is it possible to model the 1D diffusion with losses in the stationary and transient cases? Is it possible to model a coupling between percolation theory which allows building a spiral galaxy and the evolution of the SBs in the galactic plane? Can the galactic latitude and longitude cuts of observed radiation be explained by the diffusion? Do the galactic longitude cuts of observed radiation follow the sine law?

In order to answer the above questions, Section 2 reviews the connection between random walks and diffusion, Section 3 reviews stationary diffusions with losses and introduces a new stationary diffusion with losses, Section 4 introduces the new transient diffusion with losses, and Section 5.2 applies the new results about 1D diffusion to the latitude profiles of the galactic plane for the observed radiation. Section 6 reviews a model for a spiral galaxy as given by percolation theory, introduces a simple model for the SBs, models the diffusion of CRs from the SBs and finally displays the observed radiation for a spiral as seen face on, in Mollweide projection and as longitude profiles.

 2. The Random Walk

The dependence of the mean square displacement, R 2 ( t ) ¯ , according to Equation (8.38) in [18] is

R 2 ( t ) ¯ = 2 d D t   ( t → ∞ ) ,

where d is the number of spatial dimensions. From Equation (1), the diffusion coefficient is derived in the continuum:

D = ( t → ∞ ) R ¯ 2 2 d t .

Using discrete time steps, the average square radius after N steps, Equation (12.5) in [18], is

〈 R 2 ( N ) 〉 ~ 2 d D N ,

from which the diffusion coefficient is derived:

D = 〈 R 2 ( N ) 〉 2 d N .

If 〈 R 2 ( N ) 〉 ~ N , the diffusion coefficient is

D = 1 2 d λ v t r

when the step length of the walker or mean free path between successive collisions is λ and the transport velocity is v t r . The above formula allows an astrophysical evaluation of the diffusion coefficient. The mean free path is here chosen to be the gyro-radius of the relativistic ions, ρ Z . Once the energy is expressed in units of 1015 eV ( E 15 ), and the magnetic field in 10−6 Gauss ( H − 6 ) we have

ρ Z = 1.08 E 15 H − 6 Z   pc ,

where Z is the atomic number. On assuming that the CRs diffuse with a mean free path equal to the relativistic gyro-radius, the transport velocity is equal to the speed of light and d = 1 , the case here analysed, the diffusion coefficient according to Equation (5), is

D = 0.1654 E 15 Z B − 6 pc 2 year = 1.654 × 10 − 7 E G e V Z B − 6 pc 2 year . 3. The Stationary Diffusion

We now analyse the stationary 1D diffusion both in the absence and presence of losses. In the following, spatial distance is expressed in pc, the time in years, and

the diffusion coefficient in pc 2 yr .

3.1. Absence of Losses

Fick’s second law in 1D states that a change in concentration, u ( x , t ) , in any part of the system is due to an inflow and an outflow of material into and out of a part of the system:

∂ ∂ t u ( x , t ) = D ( ∂ 2 ∂ x 2 u ( x , t ) ) ,

where D is the diffusion coefficient and t is the time. For a stationary state, the above equation is

D ( ∂ 2 ∂ x 2 u ( x , t ) ) = 0.

The concentration increases from 0 at x = a to a maximum value C m at x = b and then falls again to 0 at x = c . The two solutions are

u ( x ) = C m ( a − x ) a − b   a < x < b ,

and

u ( x ) = − C m ( c − x ) b − c   b < x < c . 3.2. Presence of Losses

The presence of losses modifies Fick’s second law in 1D for the steady state, see Equation (8) as

D ( d 2 d x 2 u ( x ) ) − a l u ( x ) = 0 ,

where the parameter a l regulates the losses and is expressed in 1 year . The concentration increases from 0 at x = a to a maximum value C m at x = b and then falls again to 0 at x = c . The two solutions are

u ( x ) = C m ( e a l ( 2 a − b − x ) D − e − a l ( b − x ) D ) e 2 a l ( a − b ) D − 1 ;   a < x < b ,

and

u ( x ) = ( − e a l ( b − x ) D + e a l ( b − 2 c + x ) D ) C m e 2 a l ( b − c ) D − 1 ;   b < x < c .

The solution with a < x < b is reported in Appendix A. Figure 1 reports the new 1D theoretical solution when the coefficient of the losses is variable.

4. The Transient Diffusion with Losses

Fick’s second law in 1D in the presence of losses states that a change in concentration, u ( x , t ) , is

∂ ∂ t u ( x , t ) = D ( ∂ 2 ∂ x 2 u ( x , t ) ) − a l u ( x , t ) ,

where D is the diffusion coefficient, t is the time and the parameter a l regulates the losses. We now solve Fick’s second law in 1D over the spatial domain [ 0, L ] in the presence of an initial profile (the initial condition) for the number of particles. The first case to be analysed is an initial exponential profile of concentration

N ( x ,0 ) = N 0 e − x s L ,

where s is an adjustable parameter and N 0 the number of particles at x = 0 . The boundary conditions are assumed to be ∂ ∂ x u ( 0, t ) = 0 , ∂ ∂ x u ( L , t ) = 0 and the solution is the following Fourier series

Figure 1. Values of concentration in the case of steady state with losses computed with Equations (13) and (14) when a = −500 pc, b = 0 pc, c = 500 pc and D = 1   pc 2 yr : a l = 1.0 × 10 − 6 1 year (full line), a l = 1.0 × 10 − 5 1 year (dashed), a l = 1.0 × 10 − 4 1 year (dot-dash-dot-dash), a l = 1.0 × 10 − 3 1 year (dotted).

u ( x , t ) = 1 s ( − N 0 e − a l t e − s + N 0 e − a l t + ( ∑ n = 1 ∞ ( − 2 cos ( n π x L ) e − t ( D π 2 n 2 + L 2 a l ) L 2 s N 0 ( e − s ( − 1 ) n − 1 ) π 2 n 2 + s 2 ) ) s ) .

A 3D surface of the solution as a function of space and time is reported in Figure 2. The second case to be analysed is an initial sine profile for the concentration,

N ( x ,0 ) = N 0 sin ( π x L )

where N 0 is the number of particles at x = 0 . The boundary conditions are assumed to be ∂ ∂ x u ( 0, t ) = 0 , ∂ ∂ x u ( L , t ) = 0 and the solution is the following Fourier series

u ( x , t ) = 2 N 0 e − a l t π + ∑ n = 2 ∞ ( − 2 cos ( n π x L ) e − t ( D π 2 n 2 + L 2 a l ) L 2 N 0 ( ( − 1 ) n + 1 ) π ( n 2 − 1 ) )     .

The solution as a function of x and t is presented as a surface plot in Figure 3.

Figure 2. Values of concentration in the transient case with losses in the presence of an exponential profile as computed with Equation (17) as a function of space and time when L = 1000 pc, D = 5 × 10 − 4 pc 2 yr , s = 1.0 × 10 − 5 . N 0 = 1.0 × 10 3 and a l = 1.0 × 10 − 3 1 year .

Figure 3. Values of concentration in the transient case with losses in the presence of a sine profile as computed with Equation (19) as a function of space and time when L = 1000 pc, D = 1 × 10 − 6   pc 2 yr , N 0 = 1.0 and a l = 1.0 × 10 − 10 1 year .

An example of the influence of the parameter a l on the solution is reported in Figure 4. The third case is an initial sin4 profile for the concentration

N ( x ,0 ) = N 0 ( sin 4 ( π x L ) )

where N 0 the number of particles at x = 0 . The boundary conditions are assumed to be ∂ ∂ x u ( 0, t ) = 0 , ∂ ∂ x u ( L , t ) = 0 and the analytical solution is

u ( x , t ) = N 0 ( cos ( 4 π x L ) e − t ( 16 D π 2 + L 2 a l ) L 2 − 4 cos ( 2 π x L ) e − t ( 4 D π 2 + L 2 a l ) L 2 + 3   e − a l t ) 8 .

The solution as a function of time and space is reported in Figure 5.

Figure 4. Values of concentration in the transient case with losses in the presence of a sine profile as a function of a l when L = 1000 pc, x = 250 pc, D = 1 × 10 − 6 pc 2 yr and N 0 = 1.0 .

Figure 5. Values of concentration with losses in the presence of a sin4 profile computed with Equation (21) as function of space and time when L = 1000 pc, D = 1 × 10 − 6 pc 2 yr , N 0 = 1.0 and a l = 1.0 × 10 − 10 1 year .

 5. Astrophysical Profiles 5.1. Statistics

The merit function χ 2 is computed according to the formula

χ 2 = ∑ i = 1 n ( T i − O i ) 2 O i ,

where n is the number of elements of the sample, T i is the theoretical value, and O i is the experimental data. In the following we will compare our results with two standard types of fits. The first is the polynomial fit of degree m

y ( x ) = a 0 + a 1 x + a 2 x 2 + ⋯ + a m x m ,

where the a 1 are m + 1 unknown coefficients, see the Fortran subroutine lfit in [19]. The second fit is represented by the Gaussian function

y ( x ) = C e − ( x − x m ) 2 2 σ 2 2 2 π σ ,

where C, x m and σ are three parameters to be found with the Levenberg method, see the Fortran subroutine mrqmin in [19].

5.2. Latitude Profile

Astronomers usually report the intensity of emission in the various bands as flux versus galactic latitude or galactic longitude. In the following we will assume that the synchrotron radiation which is thought to vary from the radio to the γ region is proportional to the concentration of the diffusing CR. Further, the distance from the galactic plane, the vertical galactic height, is assumed to be proportional to the galactic latitude. We now make a comparison between the observed flux versus the galactic latitude and the theoretical behaviour of the concentration of CR as given by the diffusion. A first example is given by the γ-ray diffuse emission around 15 TeV as reported in Figure 3 in [20]. Figure 6 reports the observed data and the model of 1D diffusion with an exponential profile of concentration, χ 2 of the various models in Table 1.

A second example is given by the γ-ray diffuse emission as detected by AR-GO-YBJ in the interval [350 GeV, 2 TeV] which is reported in Figure 2 of [21]. Figure 7 reports the observed data and the model of 1D diffusion with a sine profile of concentration, χ 2 of the various models in Table 1.

Table 1. Numerical values of the parameters for the χ 2 as given by Equation (22) for different profiles and different models.

Model Reference χ 2 , Model χ 2 , Polynomial profile χ 2 , Gaussian profile
exponential profile [ 20 ] 25.35 18.5 5.1
sine profile [ 21 ] 45.27 17.97 7.25
stationary 1D [ 22 ] 176,747 931,530 337,555

Figure 6. The γ-ray flux as reported in Figure 3 of [20], inner Galaxy or 30 < l < 65 , is displayed as black points with error bar. The red full line reports the values of concentration computed with 1D diffusion in the presence of an exponential profile, see Equation (17), when L = 1000 pc, D = 4 × 10 − 3 pc 2 yr , t = 10 7   years , s = 10 5 , N 0 = 1 and a l = 10 − 6 1 year . The green dashed line represents the polynomial approximation and the blue dash-dotdash the Gaussian approximation.

Figure 7. The γ-ray flux as reported in Figure 2 of [21] is displayed as black points with error bar. The red full line reports the values of concentration computed with 1D diffusion in the presence of a sine profile, see Equation (19), when L = 1000 pc, D = 10 − 6 pc 2 yr , t = 10 7   years , N 0 = 1 and a l = 10 − 10 1 year . The green dashed line represents the polynomial approximation and the blue dash-dot-dash the Gaussian approximation.

A third example is given by the radio emission at 408 MHz as detected by Planck which is reported in Figure 4 of [22]. Figure 8 reports the observed data and the model of 1D stationary diffusion with losses, χ 2 of the various models in Table 1.

Figure 8. The radio flux at 408 MHz as reported in Figure 4 of [22] is displayed as black points with error bar. The red full line reports the values of concentration computed with 1D stationary diffusion with losses, see Equations (13) and (14), when L = 1000 pc, D = 1   pc 2 yr , C m = 1 and a l = 2.5 × 10 − 4 1 year . The green dashed line represents the polynomial approximation and the blue dash-dot-dash the Gaussian approximation.

 6. The Diffusion in a Spiral Galaxy

We now review percolation theory, a model for the evolution of SBs, the diffusion from many injection points, some elements of the theory of the image which allows building theoretical profiles of the intensity of radiation versus galactic longitude, and an evaluation for the index of galactic CRs.

6.1. Percolation

The appearance of arms can be simulated through percolation theory [23]-[28]. The fundamental hypotheses and the parameters adopted in the simulation are now reviewed.

1) The motion of a gas on the galactic plane has a constant rotational velocity, denoted by VG (in the case of spiral type Sb 218 km∙s−1). Here the velocity, VG, is expressed in units of 200 km∙s−1 and will therefore be VG = 1.39.

2) The polar simulation array made by rings and cells has a radius RG = 12 kpc. The number of rings, (59), by the multiplication of RG with the number of rings for each kpc, denoted by nring/kpc, which in our case is 5. Every ring is then made up of many cells, each one with a size on the order of the galactic thickness, ≈0.2 kpc. The parameter nring/kpc can also be found by dividing 1 kpc by the cell’s approximate size.

3) The global number of cells, 11,121, multiplied by the probability of the spontaneous formation of a new cluster, psp (for example 0.01), allows the process to start (with the previous parameters, 111 new clusters were generated). Each one of these sources has 6 new surroundings that are labeled for each ring.

4) In order to better simulate the decrease of the gas density along the radius, a stimulated probability of forming new clusters with a linear dependence by the radius, pst = a + bR, was chosen. The values a and b are found by fixing prmax (for example 0.18), the stimulated probability at the outer ring, and prmin (for example 0.24) in the inner ring; of course, prmin≥prmax. This approach is surprisingly similar to the introduction of an anisotropic probability distribution in order to better simulate certain classes of spirals [29].

5) Now, new sources are selected in each ring based on the hypothesis of different stimulated probabilities. A rotation curve is imposed so that the array rotates in the same manner as the galaxy. The procedure repeats itself n times (100); we denote by tG the age of the simulation, viz., 100 × 107 yr, where 107 yr is the astrophysical counterpart of one time step.

6) In order to prevent catastrophic growth, the process is stopped when the number of surroundings is greater than max (1000) and restarts by spontaneous probability.

7) The final number of active cells (3824) is plotted with the size, which decreases linearly with the age of the cluster. In other words, the young clusters are bigger than the old ones. Only 10 cluster ages are shown; only cells with an age of less than life (in our case 10 × 107 yr) are selected.

A typical run is shown in Figure 9 and in Table 2 we summarize the parameters used in this simulation.

Figure 9. A typical simulation of the galaxy’s arms with the parameters as in Table 2 and radius of a cluster inversely proportional to its lifetime.

Table 2. Parameters of the model.

Galactic radius 12 kpc
Rings/kpc 5
Stochastic probability 0.01
Timestep 10 7 years
Cells 11,121
Active 3894

A discussion of the location of the spiral arms and that of the peak of the total synchrotron emission can be found in [30].

 6.2. The Density Profile

The vertical density distribution of galactic H I is well-known; specifically, it has the following three component behavior as a function of z, the distance from the galactic plane in pc:

n ( z ; n 1 , n 2 , n 3 , H 1 , H 2 , H 3 ) = n 1 e − z 2 / H 1 2 + n 2 e − z 2 / H 2 2 + n 3 e − | z | / H 3 .

We took [31][32][33] n 1 = 0.395   particles cm − 3 , H 1 = 127   pc , n 2 = 0.107   particles cm − 3 , H 2 = 318   pc , n 3 = 0.064   particles cm − 3 , and H 3 = 403   pc . This distribution of galactic H I is valid in the range 0.4 ≤ R ≤ R 0 , where R 0 = 8.5   kpc and R is the distance from the galactic centre. We now fit the above profile with the following theoretical inverse square dependence on z, n t h , in Cartesian coordinates,

n t h ( z ; z 0 , n 0 ) = n 0 ( 1 + z z 0 ) − 2 ,

where n 0 is the number density of the three component medium at z = 0 and z 0 can be found by minimizing the χ 2 of the difference of the two functions (Figure 10).

 6.3. The Super-Bubbles

In spherical coordinates the density is assumed to be

ρ ( z ; z 0 , ρ 0 , θ ) = { ρ 0 r < r 0 ρ 0 ( 1 + r cos ( θ ) z 0 ) 2 r 0 < r

where the parameter z 0 fixes the scale, ρ 0 is the density at z = z 0 , and θ is the polar angle. Given a solid angle Δ Ω , the mass M 0 swept in the interval [ 0, r 0 ] is

M 0 = 1 3 ρ 0 r 0 3 Δ Ω .

Figure 10. Profiles of density versus scale height z: the inverse square profile given by Equation (26) when z 0 = 239   pc , and n 0 = 0.565   particles cm − 3 , (blue dotted line) and the three-component exponential distribution as given by Equation (25) (red full line).

The total mass swept, M ( r ; r 0 , z 0 , θ , ρ 0 , Δ Ω ) , in the interval [ 0, r ] is

M ( r ; r 0 , z 0 , θ , ρ 0 , Δ Ω ) = ( 1 3 ρ 0 r 0 3 + ρ 0 z 0 2 r ( cos ( θ ) ) 2 − 2 ρ 0 z 0 3 ln ( r cos ( θ ) + z 0 ) ( cos ( θ ) ) 3     − ρ 0 z 0 4 ( cos ( θ ) ) 3 ( r cos ( θ ) + z 0 ) − ρ 0 z 0 2 r 0 ( cos ( θ ) ) 2 + 2 ρ 0 z 0 3 ln ( r 0 cos ( θ ) + z 0 ) ( cos ( θ ) ) 3     + ρ 0 z 0 4 ( cos ( θ ) ) 3 ( r 0 cos ( θ ) + z 0 ) ) Δ Ω .

The differential equation which models the conservation of momentum is

( 1 3 ρ 0 r 0 3 + ρ 0 z 0 2 r ( t ) ( cos ( θ ) ) 2 − 2 ρ 0 z 0 3 ln ( r ( t ) cos ( θ ) + z 0 ) ( cos ( θ ) ) 3 − ρ 0 z 0 4 ( cos ( θ ) ) 3 ( r ( t ) cos ( θ ) + z 0 ) − ρ 0 z 0 2 r 0 ( cos ( θ ) ) 2 + 2 ρ 0 z 0 3 ln ( r 0 cos ( θ ) + z 0 ) ( cos ( θ ) ) 3 + ρ 0 z 0 4 ( cos ( θ ) ) 3 ( r 0 cos ( θ ) + z 0 ) ) d d t r ( t k ) − 1 3 ρ 0 r 0 3 v 0 = 0,

where the initial conditions are r = r 0 and v = v 0 when t = t 0 . The adopted astrophysical units are pc for space and year for time. The starting parameters of the inverse square model are N * , the number of SN explosions in 5.0 × 107 yr, E 51 , the energy in 1051 erg, v 0 , the initial velocity which is fixed by the bursting phase, t 0 , the initial time in yr which is equal to the bursting time, and t the proper time of the SB.

A possible set of initial values is reported in Table 3 in which the initial values of the radius and velocity are fixed by the bursting phase.

Table 3. Numerical values of the parameters for the simulation in the case of the inverse square model.

n 0 [ particles cm 3 ] 1
E 51 1
N * 5.87 × 10 8
r 0 220 pc
v 0 3500 km/s
z 0 239
t 5.95 × 10 7 yr
t 0 36,948 yr

In order to simulate the structure of the galactic plane, the same basic parameters as in Figure 9 can be chosen, but now the SBs are drawn with an equal-area Aitoff projection. In particular, a certain number of clusters will be selected through a random process according to the following formula:

selected clusters = pselect ⋅ number of clusters from percolation ,

where pselect has a probability lower than one. The final result of the simulation for the network of the SBs is reported in Figure 11.

6.4. Diffusion of CR from SB

We now model the 1D diffusion from many injection points (in the following IP) in a 3D space, disposed on NSB SBs. The rules are:

1) The first of NSB SB is chosen.

2) The IPs, for example 200, are randomly generated on the surface of the selected SB.

3) The values of concentration from the multiple diffusion, the IPs, are recorded on a 3D grid ℳ ( x , y , z ) which covers the considered 3D space.

4) At each point of ℳ ( x , y , z ) we evaluate the distance of the nearest IP

5) The value of ℳ ( x , y , z ) is computed with Formula (A.1) in the case of a steady state diffusion with losses, see Table 4, or Formula (21) in the case of transient diffusion in the presence of an initial exponential profile of concentration, see Table 5.

6) The next SB is chosen and the process restarts from point 2.

 6.5. The Image Theory

The transfer equation in the presence of emission only, see for example [34] or [35], is

d I ν d s = − k ν ζ I ν + j ν ζ ,

Figure 11. Structure of the galactic plane in the Hammer-Aitoff projection, as resulting from the SB/percolation network. The value of pselect is 0.04, corresponding to 143 selected clusters. The parameters of the inverse square model are reported in Table 3 and each SB has 200 random points on its surface.

Table 4. Numerical values of the parameters for the diffusion in the case of 1D stationary diffusion with losses, see Equations (13) and (14).

a = −1000 pc b = 0 pc c = 1000 pc D = 10 − 4 pc 2 /yr C m = 10 2 a l = 10 − 9 /year

Table 5. Numerical values of the parameters for the diffusion in the case of transient diffusion with losses computed with Equation (21).

L = 2000 pc D = 10 − 4 pc 2 /yr N 0 = 10 3 t = 3 × 10 7 year a l = 10 − 10 /year

where I ν is the specific intensity, s is the line of sight, j ν the emission coefficient, k ν a mass absorption coefficient, ζ the mass density at position s, and the index ν denotes the relevant frequency of emission. The solution to Equation (32) is

I ν ( τ ν ) = j ν k ν ( 1 − e − τ ν ( s ) ) ,

where τ ν is the optical depth at frequency ν

d τ ν = k ν ζ d s .

We now continue analysing the case of an optically thin layer in which τ ν is very small (or k ν very small); the equation of transfer is

d I ν d s = j ν ζ .

The integration of the above equation gives

I ν ( s 1 ) = I ν ( s 0 ) + ∫ s 0 s 1   j ν ζ d s .

If the background is assumed to be dark, the image is proportional to the integral of the emissivity

I ν ( s 1 ) = ∫ s 0 s 1   j ν ζ d s .

The discrete version of the above equation is

I ν ∝ ∑ 1 n   ζ ( s ) Δ s ,

where n is the number of elements belonging to the considered region. The point of view of the observer plays a significant role and we analyse three cases:

1) The Galaxy is seen face on, see Figure 12 where a theoretical annulus is visible

2) The Galaxy is seen edge on

3) Whole sky map in Hammer-Aitoff or Mollweide projection, see Figure 13.

Another interesting astrophysical feature is the annulus with enhanced synchrotron emission, whose distance from the galactic centre lies between 5.5 kpc and 7.6 kpc [30]. In Figure 14 we isolate a given region of simulated synchrotron emission.

Before continuing, we introduce the simplest model for the image of a spiral galaxy as seen edge on. We assume that the number density C of the radiationemitting material is constant in a thin cylinder (radius a s , height h, h ≪ a s ) and then falls to 0. The line of sight, when the observer is situated at the infinity of the x-axis, is the locus parallel to the x-axis which crosses the position y in a Cartesian x-y plane and terminates at the external circle of radius a s , see [36]. The length of this locus is

Figure 12. Intensity of synchrotron emission when the galaxy is face on, see parameters of the diffusion in Table 5.

Figure 13. Intensity of synchrotron emission when the Galaxy is seen in Mollweide projection, see parameters of the diffusion in Table 5.

Figure 14. Intensity map of synchrotron emission comprised between the maximum and maximum/2.1 (green zone), which has the appearance of an irregular annulus, and two radii, 5.5 kpc and 7.6 kpc (red circles) which include the observed annulus; parameters as in Figure 12.

l 0 a s = 2 × a s 2 − y 2 ;   0 ≤ y < a s .

The number density C m is constant in the thin cylinder of radius a s and therefore the intensity of the radiation is

I 0 a s ∝ C m × 2 × a 2 − y 2 ∝ C m × 2 a s sin ( θ ) ;   0 ≤ y < a s ,

where the angle θ varies between −90 deg and 90 deg. An example of the Galaxy as seen edge on is given by the radio emission at 408 MHz as detected by Planck which is reported in Figure 5 of [22], see Figure 15. We now analyse whether the sine law as represented by the above equation is comparable with standard fits. For this purpose Figure 16 reports the comparison of the radiointensity versus galactic longitude with the sine law, a polynomial fit and a Gaussian fit; the χ 2 being evaluated in Table 6.

Figure 15. Intensity of synchrotron emission in Mollweide projection, see parameters of the diffusion in Table 5 (green line), observed data as in Figure 5 of [22] (red points) and blue theoretical thick line given by the trigonometrical Equation (40).

Figure 16. Observed intensity of synchrotron emission in Mollweide projection, as in Figure 5 of [22] (black points), red theoretical thick line given by the trigonometrical Equation (40), the green dashed line represents the polynomial approximation and the blue dash-dot-dash the Gaussian approximation.

 6.6. The Spectral Index

Let us assume that the initial number of CRs that are diffusing, N, has the following dependence on the diffusion coefficient:

N = N 0 ( D / D 0 ) β ,

where β is the exponent of the power law. The analytical solution to the transient equation of diffusion with losses, Equation (15), for an initial sin4 profile of concentration is

u ( x , t ) = N 0 ( D D 0 ) β ( cos ( 4 π x L ) e − t ( 16 D π 2 + L 2 a l ) L 2 − 4 cos ( 2 π x L ) e − t ( 4 D π 2 + L 2 a l ) L 2 + 3   e − a l t ) 8 .

In the above equation the diffusion coefficient can be expressed in terms of energy in GeV, see Equation (7), by Table 7.

u ( x , t ) = ( E ( GeV ) E 0 ( GeV ) ) β × ( 0.125 N 0 e − 1.0 × 10 − 14 t ( 1.0 × 10 14 L 2 a l + 2.611 × 10 9 E ( GeV ) ) L 2 cos ( 12.566 x L )   − 0.5 N 0 e − 8.0 × 10 − 15 t ( 1.25 × 10 14 L 2 a l + 8.162 × 10 8 E ( GeV ) ) L 2 cos ( 6.283 x L ) + 0.37 N 0 e − 1.0 a l t ) .

Figure 17 reports the results of the simulation of CRs as well the data for CRs as extracted from [37].

Table 6. Numerical values of the parameters for the χ 2 as given by Equation (22) for distribution of radio-emission versus longitude.

Case Reference χ 2 , Sine model χ 2 , Polynomial profile χ 2 , Gaussian profile
radio-observations [ 22 ] 1,900,888 2,130,949 1,192,361
simulation this paper 1,384,459 1,005,467 1,192,579

Table 7. Numerical values of the parameters for the transient diffusion with losses computed with Equation (43).

L = 2000 pc x = 500 pc N 0 = 5 × 10 8 t = 3 × 10 7 year a l = 10 − 7 /year E 0 = 10 GeV β = −3

Figure 17. Flux of Hydrogen versus energy per nucleus in Gev: experimental data (green points) and theoretical power law (red full line) as given by Formula (43) with parameters as in Table 7.

 7. Conclusions

Diffusion with Stationary State

A new solution for the 1D diffusion equation with losses proportional to the concentration was derived, see Equations (13) and (14).

PDE & Boundary Conditions

Two new solutions for the transient 1D diffusion with losses in terms of Fourier series were derived. The first solution is in the presence of an exponential profile of concentration, see Equation (17), and the second solution was derived in the presence of a trigonometric profile, see Equation (19). A third analytical solution was derived in the case on an initial sin4 profile of concentration, see Equation (21).

The Astrophysical Profiles

The new laws derived for the diffusion of CRs were applied to the observed profiles of radiation versus galactic latitude, analysing two cases of diffuse γ-ray emission, see Figure 6 and Figure 7, and one case of radio emission, see Figure 8. The analysis of the χ 2 as reported in Table 1 suggests that in one of the three cases considered the analysed new physical mechanisms produces a χ 2 smaller than for the polynomial and the Gaussian fits. A longitude distribution of emission at 408 Mhz along the galactic plane as well the theoretical profile were reported in Figure 15. An analysis of the χ 2 for the observed radio-case indicates that the sine law given by Equation (40) produces a χ 2 smaller than the polynomial fit but bigger than the Gaussian fit, see first line of Table 6. In the simulated case the χ 2 is comparable but bigger than the polynomial and Gaussian fit, see the second line in Table 6. In other words we have validated a classical explanation for the excess of radiation observed in the various astronomical bands at the centre of the galaxy.

The Astrophysical Map

Figure 12 reports a map of the theoretical synchrotron emission for a spiral galaxy as seen face on. The tendency to form an annulus, such as that reported in Figure 2 in [30], is due to the combination of the spiral structure with the diffusion of CRs.

 Future Projects

The arguments here developed can be applied to the analysis of the γ-ray background, following the hypothesis that it is produced by the star-forming galaxies [38]. The SBs are hot and emit X-rays, so there are a lot of electrons for the gamma-rays to scatter and therefore the hypothesis of the inverse Compton production of radiation should be considered.

Appendix: Solution of the ODE

The ODE of the second order

D ( d 2 d x 2 u ( x ) ) − a l u ( x ) = 0,

is homogeneous and has constant coefficients. A trial solution is

u ( x ) = e r x ,

the characteristic polynomial is

D   r 2 − a l = 0,

which has roots

r 1 = a l D ,   r 2 = − a l D .

The general solution of the ODE is

u ( x ) = c 1 e a l x D D + c 2 e − a l x D D .

We now introduce two boundary conditions u ( a ) = 0 and u ( b ) = C m which yields a system of two equations in the two variables c 1 and c 2

c 1 e a l a D + c 2 e − a l a D = 0, c 1 e a l b D + c 2 e − a l b D = C m .

The two solutions of the system are

c 1 = − C m e − a l a D − e − a l a D e a l b D + e − a l b D e a l a D , c 2 = C m e a l a D − e − a l a D e a l b D + e − a l b D e a l a D ,

and therefore the solution of the ODE is

u ( x ) = C m ( e 2 a l ( a − x ) D − 1 ) e − a l ( b − x ) D e 2 a l ( a − b ) D − 1 . References Streimatter, R.E., Balasubrahmanyan, V.K., Protheroe, R.J. and Ormes, J.F. (1985) Cosmic Ray Propagation in the Local Superbubble. Astronomy&Astrophysics, 143, 249-255. Streimatter, R.E. Balasubrahmanyan, V.K. Protheroe, R.J. Ormes, J.F. 1985 Cosmic Ray Propagation in the Local Superbubble Astronomy & Astrophysics 143 Higdon, J.C., Lingenfelter, R.E. and Ramaty, R. (1998) Cosmic-Ray Acceleration from Supernova Ejecta in Superbubbles. The Astrophysical Journal, 509, L33-L36. https://doi.org/10.1086/311757 10.1086/311757https://doi.org/10.1086/311757 Higdon, J.C. Lingenfelter, R.E. Ramaty, R. 1998 Cosmic-Ray Acceleration from Supernova Ejecta in Superbubbles The Astrophysical Journal 509 10.1086/311757 Alibés, A., Labay, J. and Canal, R. (2002) Galactic Cosmic Rays from Superbubbles and the Abundances of Lithium, Beryllium, and Boron. The Astrophysical Journal, 571, 326-333. (Preprint) https://doi.org/10.1086/339937 10.1086/339937https://doi.org/10.1086/339937 Labay, J. Canal, R. Lithium, B 2002 Galactic Cosmic Rays from Superbubbles and the Abundances of Lithium, Beryllium, and Boron The Astrophysical Journal 571 10.1086/339937 Higdon, J.C. and Lingenfelter, R.E. (2003) The Superbubble Origin of 22Ne in Cosmic Rays. The Astrophysical Journal, 590, 822-832. https://doi.org/10.1086/375192 10.1086/375192https://doi.org/10.1086/375192 Higdon, J.C. Lingenfelter, R.E. 2003 The Superbubble Origin of 22Ne in Cosmic Rays The Astrophysical Journal 590 10.1086/375192 Higdon, J.C. and Lingenfelter, R.E. (2005) OB Associations, Supernova-Generated Superbubbles, and the Source of Cosmic Rays. The Astrophysical Journal, 628, 738-749. https://doi.org/10.1086/430814 10.1086/430814https://doi.org/10.1086/430814 Higdon, J.C. Lingenfelter, R.E. Associations, S 2005 OB Associations, Supernova-Generated Superbubbles, and the Source of Cosmic Rays The Astrophysical Journal 628 10.1086/430814 Lingenfelter, R.E. and Higdon, J.C. (2007) Cosmic Rays, Dust, and the Mixing of Supernova Ejecta into the Interstellar Medium in Superbubbles. The Astrophysical Journal, 660, 330-335. https://doi.org/10.1086/513420 10.1086/513420https://doi.org/10.1086/513420 Lingenfelter, R.E. Higdon, J.C. Rays, D 2007 Cosmic Rays, Dust, and the Mixing of Supernova Ejecta into the Interstellar Medium in Superbubbles The Astrophysical Journal 660 10.1086/513420 Butt, Y.M. and Bykov, A.M. (2008) A Cosmic-Ray Resolution to the Superbubble Energy Crisis. The Astrophysical Journal, 677, L21-L22. (Preprint) https://doi.org/10.1086/587875 10.1086/587875https://doi.org/10.1086/587875 Butt, Y.M. Bykov, A.M. 2008 A Cosmic-Ray Resolution to the Superbubble Energy Crisis The Astrophysical Journal 677 10.1086/587875 Ferrand, G. and Marcowith, A. (2010) On the Shape of the Spectrum of Cosmic Rays Accelerated Inside Superbubbles. Astronomy&Astrophysics, 510, Article No. A101. (Preprint) https://doi.org/10.1051/0004-6361/200913520 10.1051/0004-6361/200913520https://doi.org/10.1051/0004-6361/200913520 Ferrand, G. Marcowith, A. 2010 On the Shape of the Spectrum of Cosmic Rays Accelerated Inside Superbubbles Astronomy & Astrophysics 510 No 10.1051/0004-6361/200913520 Barghouty, A.F. and Schnee, D.A. (2012) Anomalous Transport of High-energy Cosmic Rays in Galactic Superbubbles. I. Numerical Simulations. The AstrophysicalJournal, 749, 178-188. https://doi.org/10.1088/0004-637X/749/2/178 10.1088/0004-637X/749/2/178https://doi.org/10.1088/0004-637X/749/2/178 Barghouty, A.F. Schnee, D.A. 2012 Anomalous Transport of High-energy Cosmic Rays in Galactic Superbubbles I. Numerical Simulations. The Astrophysical Journal 749 10.1088/0004-637X/749/2/178 Heesen, V., Brinks, E., Krause, M.G.H., Harwood, J.J., Rau, U., Rupen, M.P., Hunter, D.A., Chyży, K.T. and Kitchener, G. (2015) The Non-Thermal Superbubble in IC 10: The Generation of Cosmic Ray Electrons Caught in the Act. Monthly Notices of the Royal Astronomical Society: Letters, 447, L1-L5. (Preprint) https://doi.org/10.1093/mnrasl/slu168 10.1093/mnrasl/slu168https://doi.org/10.1093/mnrasl/slu168 Heesen, V. Brinks, E. Krause, M.G.H. Harwood, J.J. Rau, U. Rupen, M.P. Hunter, D.A. Kitchener, G. 2015 The Non-Thermal Superbubble in IC 10: The Generation of Cosmic Ray Electrons Caught in the Act Monthly Notices of the Royal Astronomical Society: Letters 447 10.1093/mnrasl/slu168 Gupta, S., Nath, B.B., Sharma, P. and Eichler, D. (2018) Lack of Thermal Energy in Superbubbles: Hint of Cosmic Rays? Monthly Notices of the Royal AstronomicalSociety: Letters, 473, 1537-1553. (Preprint) https://doi.org/10.1093/mnras/stx2427 10.1093/mnras/stx2427https://doi.org/10.1093/mnras/stx2427 Gupta, S. Nath, B.B. Sharma, P. Eichler, D. 2018 Lack of Thermal Energy in Superbubbles: Hint of Cosmic Rays? Monthly Notices of the Royal Astronomical Society: Letters, 473, 1537-1553 10.1093/mnras/stx2427 Lingenfelter, R.E. (2018) Cosmic Rays from Supernova Remnants and Superbubbles. AdvancesinSpaceResearch, 62, 2750-2763. (Preprint) https://doi.org/10.1016/j.asr.2017.04.006 10.1016/j.asr.2017.04.006https://doi.org/10.1016/j.asr.2017.04.006 Lingenfelter, R.E. 2018 Cosmic Rays from Supernova Remnants and Superbubbles Advances in Space Research 62 10.1016/j.asr.2017.04.006 Tolksdorf, T., Grenier, I.A., Joubaud, T. and Schlickeiser, R. (2019) Cosmic Rays in Superbubbles. The Astrophysical Journal, 879, 66-76. https://doi.org/10.3847/1538-4357/ab24c6 10.3847/1538-4357/ab24c6https://doi.org/10.3847/1538-4357/ab24c6 Tolksdorf, T. Grenier, I.A. Joubaud, T. Schlickeiser, R. 2019 Cosmic Rays in Superbubbles The Astrophysical Journal 879 10.3847/1538-4357/ab24c6 Zhang, Z., Murase, K. and Mészáros, P. (2020) Cosmic Rays Escaping from Galactic Starburst-Driven Superbubbles. Monthly Notices of the Royal Astronomical Society: Letters, 492, 2250-2260. (Preprint) https://doi.org/10.1093/mnras/staa022 10.1093/mnras/staa022https://doi.org/10.1093/mnras/staa022 Zhang, Z. Murase, K. 2020 Cosmic Rays Escaping from Galactic Starburst-Driven Superbubbles Monthly Notices of the Royal Astronomical Society: Letters 492 10.1093/mnras/staa022 Joubaud, T., Grenier, I.A., Casandjian, J.M., Tolksdorf, T. and Schlickeiser, R. (2020) The Cosmic-Ray Content of the Orion-Eridanus Superbubble. Astronomy&Astrophysics, 635, Article No. A96. (Preprint) https://doi.org/10.1051/0004-6361/201937205 10.1051/0004-6361/201937205https://doi.org/10.1051/0004-6361/201937205 Joubaud, T. Grenier, I.A. Casandjian, J.M. Tolksdorf, T. Schlickeiser, R. 2020 The Cosmic-Ray Content of the Orion-Eridanus Superbubble Astronomy & Astrophysics 635 No 10.1051/0004-6361/201937205 Vieu, T., Gabici, S., Tatischeff, V. and Ravikularaman, S. (2022) Cosmic Ray Production in Superbubbles. Monthly Notices of the Royal Astronomical Society: Letters, 512, 1275-12293. (Preprint) https://doi.org/10.1093/mnras/stac543 10.1093/mnras/stac543https://doi.org/10.1093/mnras/stac543 Vieu, T. Gabici, S. Tatischeff, V. Ravikularaman, S. 2022 Cosmic Ray Production in Superbubbles Monthly Notices of the Royal Astronomical Society: Letters 512 10.1093/mnras/stac543 Murgia, S. (2020) The Fermi-LAT Galactic Center Excess: Evidence of Annihilating Dark Matter? AnnualReviewofNuclearandParticleScience, 70, 455-483. https://doi.org/10.1146/annurev-nucl-101916-123029 10.1146/annurev-nucl-101916-123029https://doi.org/10.1146/annurev-nucl-101916-123029 Murgia, S. 2020 The Fermi-LAT Galactic Center Excess: Evidence of Annihilating Dark Matter? Annual Review of Nuclear and Particle Science, 70, 455-483 10.1146/annurev-nucl-101916-123029 Gould, H. and Tobochnik, J. (1988) An Introduction to Computer Simulation Methods. Addison-Wesley, Reading, MA. Gould, H. Tobochnik, J. Addison-Wesley, R 1988 An Introduction to Computer Simulation Methods Addison-Wesley Press, W.H., Teukolsky, S.A., Vetterling, W.T. and Flannery, B.P. (1992) Numerical Recipes in Fortran 77. The Art of Scientific Computing. Cambridge University Press, Cambridge. Press, W.H. Teukolsky, S.A. Vetterling, W.T. Flannery, B.P. Press, C 1992 Numerical Recipes in Fortran 77 The Art of Scientific Computing. Cambridge University Press Abdo, A.A., Allen, B., Aune, T., et al. (2008) A Measurement of the Spatial Distribution of Diffuse TeV Gamma-Ray Emission from the Galactic Plane with Milagro. The Astrophysical Journal, 688, 1078-1083. (Preprint) Abdo, A.A. Allen, B. Aune, T. 2008 A Measurement of the Spatial Distribution of Diffuse TeV Gamma-Ray Emission from the Galactic Plane with Milagro The Astrophysical Journal 688 Bartoli, B., Bernardini, P., Bi, X.J., et al. (2015) Study of the Diffuse Gamma-Ray Emission from the Galactic Plane with ARGO-YBJ. The Astrophysical Journal, 806, 20-31. (Preprint) Bartoli, B. Bernardini, P. Bi, X.J. 2015 Study of the Diffuse Gamma-Ray Emission from the Galactic Plane with ARGO-YBJ The Astrophysical Journal 806 Planck Collaboration, P.A.R.A., Aghanim, N., Alves, M.I.R., et al. (2015) Planck Intermediate Results. XXIII. Galactic Plane Emission Components Derived from Planck with Ancillary Data. Astronomy&Astrophysics, 580, A13-A41. (Preprint) Collaboration, P.A.R.A. Aghanim, N. Alves, M.I.R. 2015 Planck Intermediate Results XXIII. Galactic Plane Emission Components Derived from Planck with Ancillary Data. Astronomy & Astrophysics 580 Seiden, P.E. and Gerola, H. (1979) Properties of Spiral Galaxies from a Stochastic Star Formation Model. The Astrophysical Journal, 233, 56-66. https://doi.org/10.1086/157366 10.1086/157366https://doi.org/10.1086/157366 Seiden, P.E. Gerola, H. 1979 Properties of Spiral Galaxies from a Stochastic Star Formation Model The Astrophysical Journal 233 10.1086/157366 Seiden, P.E. (1983) The Role of the Gas in Propagating Star Formation. The Astrophysical Journal, 266, 555-561. Seiden, P.E. 1983 The Role of the Gas in Propagating Star Formation The Astrophysical Journal 266 Schulman, L.S. and Seiden, P.E. (1986) Percolation and Galaxies Science, 233, 425-431. https://doi.org/10.1126/science.233.4762.425 10.1126/science.233.4762.42517794566https://doi.org/10.1126/science.233.4762.425 Schulman, L.S. Seiden, P.E. 1986 Percolation and Galaxies Science, 233, 425-431 10.1126/science.233.4762.425 17794566 Zaninetti, L. (1988) Percolation and Synchrotron Emission. I—The Case of Spiral Galaxies. Astronomy&Astrophysics, 190, 17-20. Zaninetti, L. 1988 Percolation and Synchrotron Emission I—The Case of Spiral Galaxies. Astronomy & Astrophysics 190 Seiden, P.E. and Schulman, L.S. (1990) Percolation Model of Galactic Structure. AdvancesinPhysics, 39, 1-54. https://doi.org/10.1080/00018739000101461 10.1080/00018739000101461https://doi.org/10.1080/00018739000101461 Seiden, P.E. Schulman, L.S. 1990 Percolation Model of Galactic Structure Advances in Physics 39 10.1080/00018739000101461 Zaninetti, L. (2017) The Milky Way as Modeled by Percolation and Superbubbles. (Preprint) Zaninetti, L. 2017 The Milky Way as Modeled by Percolation and Superbubbles Jungwiert, B. and Palouš, J. (1994) Stochastic Self-Propagating Star Formation with Anisotropic Probability Distribution. Astronomy&Astrophysics, 287, 55-67. Jungwiert, B. 1994 Stochastic Self-Propagating Star Formation with Anisotropic Probability Distribution Astronomy & Astrophysics 287 Vallée, J.P. (2022) Superposing the Magnetic Spiral Structure of the Milky Way, on the Stellar Spiral Arms—Matching the Unique Galactic Magnetic Field Reversal Zone with Two Galactic Spiral Arm Segments. InternationalJournalofAstronomyandAstrophysics, 12, 281-300. https://doi.org/10.4236/ijaa.2022.124017 10.4236/ijaa.2022.124017https://doi.org/10.4236/ijaa.2022.124017 2022 Superposing the Magnetic Spiral Structure of the Milky Way, on the Stellar Spiral Arms—Matching the Unique Galactic Magnetic Field Reversal Zone with Two Galactic Spiral Arm Segments International Journal of Astronomy and Astrophysics 12 10.4236/ijaa.2022.124017 Bisnovatyi-Kogan, G.S. and Silich, S.A. (1995) Shock-Wave Propagation in the Nonuniform Interstellar Medium. Reviews of Modern Physics, 67, 661-712. https://doi.org/10.1103/RevModPhys.67.661 10.1103/RevModPhys.67.661https://doi.org/10.1103/RevModPhys.67.661 Bisnovatyi-Kogan, G.S. Silich, S.A. 1995 Shock-Wave Propagation in the Nonuniform Interstellar Medium Reviews of Modern Physics 67 10.1103/RevModPhys.67.661 Dickey, J.M. and Lockman, F.J. (1990) H I in the Galaxy. Annual Review of Astronomy and Astrophysics, 28, 215-259. https://doi.org/10.1146/annurev.aa.28.090190.001243 10.1146/annurev.aa.28.090190.001243https://doi.org/10.1146/annurev.aa.28.090190.001243 Dickey, J.M. Lockman, F.J. 1990 H I in the Galaxy Annual Review of Astronomy and Astrophysics 28 10.1146/annurev.aa.28.090190.001243 Lockman, F.J. (1984) The H I Halo in the Inner Galaxy. The Astrophysical Journal, 283, 90-97. https://doi.org/10.1086/162277 10.1086/162277https://doi.org/10.1086/162277 Lockman, F.J. 1984 The H I Halo in the Inner Galaxy The Astrophysical Journal 283 10.1086/162277 Rybicki, G. and Lightman, A. (1991) Radiative Processes in Astrophysics. Wiley-Interscience, New York. Rybicki, G. Lightman, A. Wiley-Interscience, N 1991 Radiative Processes in Astrophysics Wiley-Interscience Hjellming, R.M. (1988) Radio Stars. In: Verschuur, G.L. and Kellermann, K.I., Eds., Galactic and Extragalactic Radio Astronomy, Astronomy and Astrophysics Library, Springer-Verlag, Berlin, 381-438. https://doi.org/10.1007/978-1-4612-3936-9_9 10.1007/978-1-4612-3936-9_9https://doi.org/10.1007/978-1-4612-3936-9_9 Hjellming, R.M. Verschuur, G.L. Kellermann, K.I. Astronomy, A Library, S Verlag, B 1988 Radio Stars In: Verschuur 381 10.1007/978-1-4612-3936-9_9 Zaninetti, L. (2009) Scaling for the Intensity of Radiation in Spherical and Aspherical Planetary Nebulae. Monthly Notices of the Royal Astronomical Society: Letters, 395, 667-697. https://doi.org/10.1111/j.1365-2966.2009.14551.x 10.1111/j.1365-2966.2009.14551.xhttps://doi.org/10.1111/j.1365-2966.2009.14551.x Zaninetti, L. 2009 Scaling for the Intensity of Radiation in Spherical and Aspherical Planetary Nebulae Monthly Notices of the Royal Astronomical Society: Letters 395 10.1111/j.1365-2966.2009.14551.x Zyla, P., et al. (Particle Data Group) (2020) Review of Particle Physics. PTEP: Progress of Theoretical and Experimental Physics, 2020, 083C01. Zyla, P. 2020 Review of Particle Physics PTEP: Progress of Theoretical and Experimental Physics 2020 Roth, M.A., Krumholz, M.R., Crocker, R.M. and Celli, S. (2021) The Diffuse γ-Ray Background Is Dominated by Star-Forming Galaxies. Nature, 597, 341-344. (Preprint) https://doi.org/10.1038/s41586-021-03802-x 10.1038/s41586-021-03802-x34526703https://doi.org/10.1038/s41586-021-03802-x Roth, M.A. Krumholz, M.R. Crocker, R.M. Celli, S. 2021 The Diffuse γ-Ray Background Is Dominated by Star-Forming Galaxies Nature 597 10.1038/s41586-021-03802-x 34526703