Driving asymmetric red supergiant winds with binary interactions
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F24%3A10491436" target="_blank" >RIV/00216208:11320/24:10491436 - isvavai.cz</a>
Result on the web
<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=mK.BFd.sY7" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=mK.BFd.sY7</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1093/mnras/stae1379" target="_blank" >10.1093/mnras/stae1379</a>
Alternative languages
Result language
angličtina
Original language name
Driving asymmetric red supergiant winds with binary interactions
Original language description
Massive stars in the red supergiant (RSG) phase are known to undergo strong mass-loss through winds and observations indicate that a substantial part of this mass-loss could be driven by localized and episodic outflows. Various mechanisms have been considered to explain this type of mass-loss in RSGs, but these models often focus on single-star evolution. However, massive stars commonly evolve in binary systems, potentially interacting with their companions. Motivated by observations of the highly asymmetric circumstellar ejecta around the RSG VY CMa, we investigate a scenario where a companion on an eccentric orbit grazes the surface of an RSG at periastron. The companion ejects part of the outer RSG envelope, which radiatively cools, reaching the proper conditions for dust condensation and eventually giving rise to dust-driven winds. Using simple treatments for radiative cooling and dust-driven winds, we perform three-dimensional smoothed particle hydrodynamic simulations of this scenario with a 20 M-circle dot RSG and a 2M(circle dot) companion. We follow the evolution of the binary throughout a total of 14 orbits and observe that the orbit tightens after each interaction, in turn enhancing the mass-loss of subsequent interactions. We show that one such grazing interaction yields outflows of 3 x 10(-4)M(circle dot), which later results in wide asymmetric dusty ejecta, carrying a total mass of 0.185 M-circle dot by the end of simulations. We discuss the implications for the evolution of the binary, potential observational signatures, as well as future improvements of the model required to provide sensible predictions for the evolution of massive binaries.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - 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)
Result continuities
Project
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Continuities
S - Specificky vyzkum na vysokych skolach<br>I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace
Others
Publication year
2024
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Monthly Notices of the Royal Astronomical Society
ISSN
0035-8711
e-ISSN
1365-2966
Volume of the periodical
531
Issue of the periodical within the volume
3
Country of publishing house
GB - UNITED KINGDOM
Number of pages
15
Pages from-to
3391-3405
UT code for WoS article
001241666000001
EID of the result in the Scopus database
2-s2.0-85195695683