Wind inhibition in HMXBs: the effect of clumping and implications for X-ray luminosity

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216224%3A14310%2F19%3A00114099" target="_blank" >RIV/00216224:14310/19:00114099 - isvavai.cz</a>

Výsledek na webu

<a href="https://doi.org/10.1017/S1743921318007573" target="_blank" >https://doi.org/10.1017/S1743921318007573</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1017/S1743921318007573" target="_blank" >10.1017/S1743921318007573</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Wind inhibition in HMXBs: the effect of clumping and implications for X-ray luminosity

Popis výsledku v původním jazyce

Winds of hot stars are driven by the radiative force due to absorption of light in the lines of heavier elements. Consequently, the mass-loss rate and the wind velocity depend on the ionization state of the wind. As a result of this, there is a feedback between the ionizing X-ray source and the stellar wind in HMXBs powered by wind accretion. We study the influence of the small-scale wind structure (clumping) on this feedback using our NLTE hydrodynamical wind models. We find that clumping weakens the effect of X-ray irradiation. Moreover, we show that the observed X-ray luminosities of HMXBs can not be explained by wind accretion scenario without introducing the X-ray feedback. Taking into account the feedback, the observed and estimated X-ray luminosities nicely agree. We identify two cases of X-ray feedback with low and high X-ray luminosities that can explain the dichotomy between SFXTs and sgXBs.

Název v anglickém jazyce

Wind inhibition in HMXBs: the effect of clumping and implications for X-ray luminosity

Popis výsledku anglicky

Winds of hot stars are driven by the radiative force due to absorption of light in the lines of heavier elements. Consequently, the mass-loss rate and the wind velocity depend on the ionization state of the wind. As a result of this, there is a feedback between the ionizing X-ray source and the stellar wind in HMXBs powered by wind accretion. We study the influence of the small-scale wind structure (clumping) on this feedback using our NLTE hydrodynamical wind models. We find that clumping weakens the effect of X-ray irradiation. Moreover, we show that the observed X-ray luminosities of HMXBs can not be explained by wind accretion scenario without introducing the X-ray feedback. Taking into account the feedback, the observed and estimated X-ray luminosities nicely agree. We identify two cases of X-ray feedback with low and high X-ray luminosities that can explain the dichotomy between SFXTs and sgXBs.

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

1743-9213

e-ISSN

—

Počet stran výsledku

6

Strana od-do

28-33

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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