Modeling of interactions between supernovae ejecta and aspherical circumstellar environments

TL;DR

This paper models the complex interactions between supernova ejecta and aspherical circumstellar environments, revealing how geometry influences shock dynamics, density structures, and instabilities in these astrophysical phenomena.

Contribution

It introduces a new hydrodynamic simulation code to analyze supernova ejecta interactions with aspherical circumstellar matter, emphasizing the effects of disk geometry and density.

Findings

Asphericity significantly affects shock and density structures.

Kelvin-Helmholtz instabilities develop at shear zones.

Disk geometry influences the thermal and dynamical evolution.

Abstract

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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