Self-similar Blast Wave for A Two-component Fluid with Variable Adiabatic Index. (arXiv:2001.03716v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_Y/0/1/0/all/0/1">Yiran Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liang_E/0/1/0/all/0/1">Edison Liang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_S/0/1/0/all/0/1">Siming Liu</a>
We propose a self-similar (SS) solution to hydrodynamic non-relativistic flow
behind a spherical strong blast wave (BW) passing through a homogeneous plasma
with efficient relativistic particle acceleration at the shock front. The flow
is described by an ideal two-fluid model with a relativistic component so that
the post-shock gas has an effective SS adiabatic index $ gamma $ varying from
$ 5/3 $ to $ 4/3 $. This solution is calculated numerically and compared with
the standard Sedov solution. We find that the BW center in our solution is
dominated by the relativistic component with $ gamma =4/3 $ for the divergence
of expansion there, and the relativistic component dominates the interior for a
moderate acceleration efficiency at the shock front. The overall efficiency of
relativistic particle acceleration can be enhanced by a factor of $ 2 $ due to
the slower adiabatic energy loss rate of the relativistic component during
expansion. Tendency of the dominance by the relativistic component may be
common in expanding astrophysical two-fluid systems such as supernova remnants,
lobes of radio galaxies.
We propose a self-similar (SS) solution to hydrodynamic non-relativistic flow
behind a spherical strong blast wave (BW) passing through a homogeneous plasma
with efficient relativistic particle acceleration at the shock front. The flow
is described by an ideal two-fluid model with a relativistic component so that
the post-shock gas has an effective SS adiabatic index $ gamma $ varying from
$ 5/3 $ to $ 4/3 $. This solution is calculated numerically and compared with
the standard Sedov solution. We find that the BW center in our solution is
dominated by the relativistic component with $ gamma =4/3 $ for the divergence
of expansion there, and the relativistic component dominates the interior for a
moderate acceleration efficiency at the shock front. The overall efficiency of
relativistic particle acceleration can be enhanced by a factor of $ 2 $ due to
the slower adiabatic energy loss rate of the relativistic component during
expansion. Tendency of the dominance by the relativistic component may be
common in expanding astrophysical two-fluid systems such as supernova remnants,
lobes of radio galaxies.
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