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

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216224%3A14310%2F19%3A00107917" target="_blank" >RIV/00216224:14310/19:00107917 - isvavai.cz</a>

Výsledek na webu

<a href="https://www.cambridge.org/core/journals/proceedings-of-the-international-astronomical-union/article/modeling-of-hydrodynamic-processes-within-highmass-xray-binaries/E1B9FB24CB1909F5CAF3FEAEC4289AC2" target="_blank" >https://www.cambridge.org/core/journals/proceedings-of-the-international-astronomical-union/article/modeling-of-hydrodynamic-processes-within-highmass-xray-binaries/E1B9FB24CB1909F5CAF3FEAEC4289AC2</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1017/S1743921319000024" target="_blank" >10.1017/S1743921319000024</a>

Jazyk výsledku

angličtina

Název v původním jazyce

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

Popis výsledku v původním jazyce

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.

Název v anglickém jazyce

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

Popis výsledku anglicky

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.

Druh

D - Stať ve sborníku

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA18-05665S" target="_blank" >GA18-05665S: Ztráta hmoty v pozdních fázích vývoje hmotných hvězd</a><br>

Návaznosti

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

Rok uplatnění

2019

Kód důvěrnosti údajů

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

Název statě ve sborníku

Symposium S346 (High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects)

ISBN

—

ISSN

1939-7291

e-ISSN

—

Počet stran výsledku

5

Strana od-do

197-201

Název nakladatele

Cambridge University Press

Místo vydání

USA

Místo konání akce

Vienna, Austria

Datum konání akce

27. 8. 2018

Typ akce podle státní příslušnosti

WRD - Celosvětová akce

Kód UT WoS článku

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