Modeling of hydrodynamic processes within high-mass X-ray
binaries

D 2019

Modeling of hydrodynamic processes within high-mass X-ray binaries

KURFÜRST, Petr a Jiří KRTIČKA

Základní údaje

Originální název

Modeling of hydrodynamic processes within high-mass X-ray binaries

Autoři

KURFÜRST, Petr (203 Česká republika, garant, domácí) a Jiří KRTIČKA (203 Česká republika, domácí)

Vydání

USA, Symposium S346 (High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects), od s. 197-201, 5 s. 2019

Nakladatel

Cambridge University Press

Další údaje

Jazyk

angličtina

Typ výsledku

Stať ve sborníku

Obor

10308 Astronomy

Stát vydavatele

Spojené státy

Utajení

není předmětem státního či obchodního tajemství

Forma vydání

elektronická verze "online"

Odkazy

URL

Impakt faktor

Impact factor: 0.905

Kód RIV

RIV/00216224:14310/19:00107917

Organizační jednotka

Přírodovědecká fakulta

ISSN

DOI

http://dx.doi.org/10.1017/S1743921319000024

Klíčová slova anglicky

massive stars; evolution; mass-loss; accretion; supernovae

Štítky

rivok

Příznaky

Mezinárodní význam, Recenzováno

Změněno: 15. 4. 2020 21:30, Mgr. Marie Šípková, DiS.

Anotace

V originále

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.

Návaznosti

GA18-05665S, projekt VaV

Název: Ztráta hmoty v pozdních fázích vývoje hmotných hvězd

Investor: Grantová agentura ČR, Ztráta hmoty v pozdních fázích vývoje hmotných hvězd

Citovat

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. 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.

@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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