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@inproceedings{1598720,
author = {Kurfürst, Petr and Krtička, Jiří},
address = {USA},
booktitle = {Symposium S346 (High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects)},
doi = {http://dx.doi.org/10.1017/S1743921319000024},
editor = {L.M.Oskinova, E.Bozzo, T.Bulik, D.Gies},
keywords = {massive stars; evolution; mass-loss; accretion; supernovae},
howpublished = {elektronická verze "online"},
language = {eng},
location = {USA},
pages = {197-201},
publisher = {Cambridge University Press},
title = {Modeling of hydrodynamic processes within high-mass X-ray binaries},
url = {https://www.cambridge.org/core/journals/proceedings-of-the-international-astronomical-union/article/modeling-of-hydrodynamic-processes-within-highmass-xray-binaries/E1B9FB24CB1909F5CAF3FEAEC4289AC2},
year = {2019}
}
TY - JOUR
ID - 1598720
AU - Kurfürst, Petr - Krtička, Jiří
PY - 2019
TI - Modeling of hydrodynamic processes within high-mass X-ray binaries
PB - Cambridge University Press
CY - USA
KW - massive stars
KW - evolution
KW - mass-loss
KW - accretion
KW - supernovae
UR - https://www.cambridge.org/core/journals/proceedings-of-the-international-astronomical-union/article/modeling-of-hydrodynamic-processes-within-highmass-xray-binaries/E1B9FB24CB1909F5CAF3FEAEC4289AC2
L2 - https://www.cambridge.org/core/journals/proceedings-of-the-international-astronomical-union/article/modeling-of-hydrodynamic-processes-within-highmass-xray-binaries/E1B9FB24CB1909F5CAF3FEAEC4289AC2
N2 - High-mass X-ray binaries belong to the brightest objects in the X-ray sky. They usually consist of a massive O or B star or a blue supergiant while the compact X-ray emitting component is a neutron star (NS) or a black hole. Intensive matter accretion onto the compact object can take place through different mechanisms: wind accretion, Roche-lobe overflow, or circumstellar disk. In our multi-dimensional models we perform numerical simulations of the accretion of matter onto a compact companion in case of Be/X-ray binaries. Using Bondi-Hoyle-Littleton approximation, we estimate the NS accretion rate. We determine the Be/X-ray binary disk hydrodynamic structure and compare its deviation from isolated Be stars’ disk. From the rate and morphology of the accretion flow and the X-ray luminosity we improve the estimate of the disk mass-loss rate. We also study the behavior of a binary system undergoing a supernova explosion, assuming a blue supergiant progenitor with an aspherical circumstellar environment.
ER -
KURFÜRST, Petr a Jiří KRTIČKA. Modeling of hydrodynamic processes within high-mass X-ray binaries. Online. In L.M.Oskinova, E.Bozzo, T.Bulik, D.Gies. \textit{Symposium S346 (High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects)}. USA: Cambridge University Press, 2019, s.~197-201. ISSN~1939-7291. Dostupné z: https://dx.doi.org/10.1017/S1743921319000024.
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