In classical mechanics, motion is modeled by the second law of Newton

where F is the force, m is the mass, and a is the acceleration. As an example, the trajectory, x ( t ) , in the presence of a constant force along the X-axis is

In special relativity, the equation of motion is

where F is the force acting on the point with momentum p , which is

where m is the rest mass and

We now analyze the case of a particle in the presence of a constant force F in 1D. We start from the relativistic equation of motion (3) and we derive the velocity when v ( 0 ) = 0

We then find the trajectory when x = 0 at t = 0

The alternative theory of relativity is characterized by an equation of motion, which is

where x is the position, a is the acceleration, F is the force, and m is the mass, see Equation (55) in [8]. In this case, the acceleration is in the same direction as the force. We now analyze the case of a particle in the presence of a constant force F in 1D. We start from the above alternative relativistic equation of motion and we derive the velocity when v ( 0 ) = 0

where tanh is the hyperbolic tangent. The 1D trajectory in alternative relativity when x = 0 at t = 0 is

where cosh is the hyperbolic cosine. The three solutions for the 1D motion in the presence of a constant force are presented in Figure 1 when F = 1 , c = 1 and m = 1 .

Figure 1. Plot of the classical solution, Equation (2), (green line), relativistic solution, Equation (7), (red line) and solution in alternative relativity, Equation (10), (blue line).

We now analyze one-dimensional motion with a resistive force of Stokes’s type [9], F r e s = − A m v ( t ) , where A is a constant. The equation that governs the motion, according to Equation (8), is

and the solution is

where v 0 is the velocity at t = t 0 . The 1D trajectory in alternative relativity can be derived from the indefinite integral, I ( t ) , of the previous equation, which is

and therefore

where x = x 0 at t = t 0 and arctanh is the inverse of the hyperbolic tangent function. We now derive the time as a function of position from the above equation

The velocity as a function of the spatial variables can be derived as

where

with tanh being the hyperbolic tangent function. In the case of a resistive force of Stokes’s type in the framework of special relativity, a solution for the velocity exists in an implicit form, see Equation (7) in [10]. A comparison between velocity as a function of time in alternative and special relativity is presented in Figure 2: the velocity in special relativity decreases more quickly than in the alternative relativity.

Figure 2. Plot of the velocity as a function of time for a resistive force of Stokes’s type, see Equation (12), (red line) and in special relativity (blue line). The parameters are A = 7 , m = 1 , β 0 = v 0 c = 0.99 , t 0 = 10 − 4 yr and r 0 = 10 − 4 pc.

In theclassical case, the rate L m of the transfer of mechanical energy is

where ρ ( t ) , r ( t ) and v ( t ) are the temporary density, radius and velocity of the SN. We assume that the density in front of the advancing expansion scales as

where r 0 is the radius at t 0 and d is a parameter which allows matching the observations; as an example, a value of d = 3 is reported in [11]. With the above assumption, the mechanical luminosity is

The energy fraction, L ν , of the mechanical luminosity deposited in the frequency ν is assumed to be proportional to the mechanical luminosity through a constant ϵ ν

The flux at frequency ν and distance D is

For practical purposes, we impose a match between the observed luminosity, L o b s , and the theoretical luminosity, L m ,

where C o b s is a constant which equalizes the observed and the theoretical luminosity and varies on the basis of the selected astronomical band. In an analogous way, the observed absolute magnitude is

where Δ m is a constant. In therelativistic case, the rate L m , r of transfer of mechanical energy, assuming the same scaling for the density in the advancing layer, is

where β ( t ) = v ( t ) c , for more details, see [12]. The conversion in magnitude of the above formula is the same as for Equation (24).

The presence of the absorption can be parametrized by introducing a slab of optical thickness τ ν . The emergent intensity I ν after the entire slab is

where S ν is a uniform source function. Integration gives

see Formula (1.30) in [13]. In the case of an optically thin medium, τ ν = ∞ , the observed luminosity can be derived from Equation (23), but otherwise, the following equation should be used:

where τ ν is a function of time. For the case of the apparent magnitude, we have

The value of τ ν can be derived with the following equation:

where m t h e o and m o b s represent the theoretical and the observed apparent magnitude. Due to the complexity of the time dependence of τ ν , a polynomial approximation of degree M is used:

with more details in [14]. In some cases, we apply the logarithms to the pair of data, i.e., log 10 ( x i ) and log 10 ( y i ) ; we call this the logarithmic polynomial approximation.

The absorption in the relativistic case is assumed to be the same once the classical luminosity, L m , is replaced by the relativistic luminosity L m , r

and

The SN here analyzed is SN 1993J, for which the temporary radius of expansion has been measured for ≈ 10 yr in the radio band [15][16]. A comparison between the observed trajectory and theoretical behavior in the framework of the alternative relativity is presented in Figure 3.

Figure 3. Theoretical radius as given by Equation (14), v 0 = 13800 km/s, t 0 = 0.1 yr, x 0 = 0.003 pc, and A m = 0.07 .

Figure 4 presents the decay of the R magnitude of SN 1993J, which is type Ii, as well as our theoretical curve.

Figure 4. The R light curve of SN 1993J over 10 yr (empty stars) and theoretical curve as given by Equation (25) (full line). Parameters of the trajectory as in Figure 3, d = 7 , Δ m = 5 and ρ 0 = 1 . The data were extracted by the author from Figure 5 in [17].

Figure 5. The H − α and the 2.0 - 8.0 eV luminosities in units of 10³⁸ ergs of SN 1993J over 10 yr (empty stars) and theoretical curve as given by Equation (25) (full line). Parameters of the trajectory as in Figure 3, d = 3 and ρ 0 = 1 . Data extracted by the author from Figure 5 of [18].

We present the H − α with soft and hard band X-ray luminosities as well as the theoretical luminosity in Figure 5; the two luminosities are matched in such a way that the maximum of both is at 123 × 10³⁸ ergs.

In the last years, the mid-infrared (mid-IR) wavelengths have also become detectable [19], and this allows comparing the theoretical light curve with the observed one in the so-called IR cold region, see Figure 6.

Figure 6. The IR cold luminosities in units of 10³⁸ ergs of SN 1993J over 10 yr (empty stars) and theoretical curve as given by Equation (25) (full line). Parameters of the trajectory as in Figure 3, d = 4.5 and ρ 0 = 1 . Data extracted by the author from Figure 5 of [19].

Figure 7 presents the radio flux density of SN 1993J at 15.2 GHz observed by the Lyle Telescope, as well as the theoretical flux, which requires a time-dependent evaluation of the optical depth τ ν , see Figure 8.

Figure 7. The radio flux density of SN 1993J over 443 days (empty stars) and theoretical curve as given by Equation (25) (full line). Parameters of the trajectory as in Figure 3, d = 3 and ρ 0 = 1 .

Figure 8. The time dependence of τ ν (empty stars) and a polynomial approximation of degree 4 (full line). Parameters as in Figure 7.