The full evolution of supernova remnants in low and high density ambient media. (arXiv:1906.10234v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Jimenez_S/0/1/0/all/0/1">Santiago Jimenez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tenorio_Tagle_G/0/1/0/all/0/1">Guillermo Tenorio-Tagle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Silich_S/0/1/0/all/0/1">Sergiy Silich</a>
Supernova explosions and their remnants (SNRs) drive important feedback
mechanisms that impact considerably the galaxies that host them. Then, the
knowledge of the SNRs evolution is of paramount importance in the understanding
of the structure of the interstellar medium (ISM) and the formation and
evolution of galaxies. Here we study the evolution of SNRs in homogeneous
ambient media from the initial, ejecta-dominated phase, to the final,
momentum-dominated stage. The numerical model is based on the Thin-Shell
approximation and takes into account the configuration of the ejected gas and
radiative cooling. It accurately reproduces well known analytic and numerical
results and allows one to study the SNR evolution in ambient media with a wide
range of densities $n_{0}$. It is shown that in the high density cases, strong
radiative cooling alters noticeably the shock dynamics and inhibits the
Sedov-Taylor stage, thus limiting significantly the feedback that SNRs provide
to such environments. For $n_{0}>5 times 10^{5}$ cm$^{-3}$, the reverse shock
does not reach the center of the explosion due to the rapid fall of the thermal
pressure in the shocked gas caused by strong radiative cooling.
Supernova explosions and their remnants (SNRs) drive important feedback
mechanisms that impact considerably the galaxies that host them. Then, the
knowledge of the SNRs evolution is of paramount importance in the understanding
of the structure of the interstellar medium (ISM) and the formation and
evolution of galaxies. Here we study the evolution of SNRs in homogeneous
ambient media from the initial, ejecta-dominated phase, to the final,
momentum-dominated stage. The numerical model is based on the Thin-Shell
approximation and takes into account the configuration of the ejected gas and
radiative cooling. It accurately reproduces well known analytic and numerical
results and allows one to study the SNR evolution in ambient media with a wide
range of densities $n_{0}$. It is shown that in the high density cases, strong
radiative cooling alters noticeably the shock dynamics and inhibits the
Sedov-Taylor stage, thus limiting significantly the feedback that SNRs provide
to such environments. For $n_{0}>5 times 10^{5}$ cm$^{-3}$, the reverse shock
does not reach the center of the explosion due to the rapid fall of the thermal
pressure in the shocked gas caused by strong radiative cooling.
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