Detailed Information on Publication Record
2019
Modeling of interactions between supernovae ejecta and aspherical circumstellar environments
KURFÜRST, Petr and Jiří KRTIČKABasic information
Original name
Modeling of interactions between supernovae ejecta and aspherical circumstellar environments
Authors
KURFÜRST, Petr (203 Czech Republic, guarantor, belonging to the institution) and Jiří KRTIČKA (203 Czech Republic, belonging to the institution)
Edition
Astronomy and Astrophysics, Les Ulis, EDP SCIENCES S A, 2019, 1432-0746
Other information
Language
English
Type of outcome
Článek v odborném periodiku
Field of Study
10308 Astronomy
Country of publisher
United States of America
Confidentiality degree
není předmětem státního či obchodního tajemství
References:
Impact factor
Impact factor: 5.636
RIV identification code
RIV/00216224:14310/19:00107336
Organization unit
Faculty of Science
UT WoS
000466697700002
Keywords in English
supernovae: general -- stars: mass-loss -- stars: circumstellar matter -- stars: evolution -- hydrodynamics
Tags
Tags
International impact, Reviewed
Změněno: 1/4/2020 15:30, Mgr. Marie Šípková, DiS.
Abstract
V originále
Massive stars are characterized by a significant loss of mass either via (nearly) 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. Since a significant fraction of most massive stars end their lives by a core collapse, supernovae (SNe) are always located inside large 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 grid-based Eulerian multidimensional hydrodynamic code built with a finite volumes method. The code is based on a directionally unsplit Roe's method that is highly efficient for calculations of shocks and physical flows with large discontinuities. We simulate a SNe explosion as a spherically symmetric blast wave. The initial geometry of the disks corresponds to a density structure of a material that orbits in Keplerian trajectories. We examine the behavior of basic hydrodynamic characteristics, i.e., the density, pressure, velocity of expansion, and temperature structure in the interaction zone under various geometrical configurations and various initial densities of CSM. We calculate the evolution of the SN - CSM system and the rate of aspherical deceleration as well as the degree of anisotropy in density, pressure, and temperature distribution. Our simulations reveal significant asphericity of the expanding envelope above all in the case of dense equatorial disks. Our ``low density'' model however also 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.
Links
| GA16-01116S, research and development project |
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| LM2010005, research and development project |
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