Modeling of interactions between supernovae ejecta and aspherical circumstellar environments. (arXiv:1904.01312v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Kurfurst_P/0/1/0/all/0/1">Petr Kurfürst</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Krticka_J/0/1/0/all/0/1">Jiří Krtička</a>
Massive stars are characterized by a significant loss of mass either via
spherically symmetric stellar winds or pre-explosion pulses, or by aspherical
forms of circumstellar matter (CSM) such as bipolar lobes or outflowing
circumstellar equatorial disks. A significant fraction of most massive stars
end their lives by a core collapse; supernovae (SNe) are always located inside
circumstellar envelopes created by their progenitors. We study the dynamics and
thermal effects of collision between expanding ejecta of SNe and CSM that may
be formed during, for example, a sgB[e] star phase, a luminous blue variable
phase, around PopIII stars, or by various forms of accretion. For
time-dependent hydrodynamic modeling we used our own code built with a finite
volumes method. The code is highly efficient for calculations of shocks and
physical flows with large discontinuities. The initial geometry of the disks
corresponds to a density structure of a material that orbits in Keplerian
trajectories. We examine the behavior of the density, pressure, velocity of
expansion, and temperature structure in the interaction zone under various
geometrical configurations of dense equatorial disks. Our `low density’ model
shows significant asphericity in the case of the disk mass-loss rate
$dot{M}_text{csd}=10^{-6},M_odot,text{yr}^{-1}$. The models also show the
zones of overdensity in the SN – disk contact region and indicate the
development of Kelvin-Helmholtz instabilities within the zones of shear between
the disk and the more freely expanding material outside the disk.
Massive stars are characterized by a significant loss of mass either via
spherically symmetric stellar winds or pre-explosion pulses, or by aspherical
forms of circumstellar matter (CSM) such as bipolar lobes or outflowing
circumstellar equatorial disks. A significant fraction of most massive stars
end their lives by a core collapse; supernovae (SNe) are always located inside
circumstellar envelopes created by their progenitors. We study the dynamics and
thermal effects of collision between expanding ejecta of SNe and CSM that may
be formed during, for example, a sgB[e] star phase, a luminous blue variable
phase, around PopIII stars, or by various forms of accretion. For
time-dependent hydrodynamic modeling we used our own code built with a finite
volumes method. The code is highly efficient for calculations of shocks and
physical flows with large discontinuities. The initial geometry of the disks
corresponds to a density structure of a material that orbits in Keplerian
trajectories. We examine the behavior of the density, pressure, velocity of
expansion, and temperature structure in the interaction zone under various
geometrical configurations of dense equatorial disks. Our `low density’ model
shows significant asphericity in the case of the disk mass-loss rate
$dot{M}_text{csd}=10^{-6},M_odot,text{yr}^{-1}$. The models also show the
zones of overdensity in the SN – disk contact region and indicate the
development of Kelvin-Helmholtz instabilities within the zones of shear between
the disk and the more freely expanding material outside the disk.
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