Modeling of interactions between supernovae ejecta and aspherical circumstellar environments

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216224%3A14310%2F19%3A00107336" target="_blank" >RIV/00216224:14310/19:00107336 - isvavai.cz</a>

Alternative codes found

RIV/00216208:11320/19:10405621

Result on the web

<a href="http://dx.doi.org/10.1051/0004-6361/201833429" target="_blank" >http://dx.doi.org/10.1051/0004-6361/201833429</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/201833429" target="_blank" >10.1051/0004-6361/201833429</a>

Result language

angličtina

Original language name

Modeling of interactions between supernovae ejecta and aspherical circumstellar environments

Original language description

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.

Czech name

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Czech description

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Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

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OECD FORD branch

10308 - Astronomy (including astrophysics,space science)

Project

Result was created during the realization of more than one project. More information in the Projects tab.

Continuities

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)<br>S - Specificky vyzkum na vysokych skolach

Publication year

2019

Confidentiality

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Name of the periodical

Astronomy and Astrophysics

ISSN

1432-0746

e-ISSN

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Volume of the periodical

625

Issue of the periodical within the volume

A24

Country of publishing house

US - UNITED STATES

Number of pages

16

Pages from-to

1-16

UT code for WoS article

000466697700002

EID of the result in the Scopus database

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