Energy Conservation in the thin layer approximation: III. The spherical relativistic case for supernovae. (arXiv:2010.10240v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Zaninetti_L/0/1/0/all/0/1">Lorenzo Zaninetti</a>
The theory of the conservation of energy in the thin layer approximation has
been extended to special relativity. Four models for the density of the
circumstellar medium are analyzed, which are represented by constant, power
law, exponential and Emden (n=5) profile for density. The astrophysical results
are presented in a numerical way, except for a Taylor expansion of the four
trajectories in the surrounding of the origin. The free parameters of the
models are particularized for SN1993j, for which the radius versus time is
known. Some evaluations on the time dilation are presented.
The theory of the conservation of energy in the thin layer approximation has
been extended to special relativity. Four models for the density of the
circumstellar medium are analyzed, which are represented by constant, power
law, exponential and Emden (n=5) profile for density. The astrophysical results
are presented in a numerical way, except for a Taylor expansion of the four
trajectories in the surrounding of the origin. The free parameters of the
models are particularized for SN1993j, for which the radius versus time is
known. Some evaluations on the time dilation are presented.
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