NLTE models of line-driven stellar winds III. Influence of X-ray radiation on wind structure of O stars

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216224%3A14310%2F09%3A00028478" target="_blank" >RIV/00216224:14310/09:00028478 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/67985815:_____/09:00333237

Výsledek na webu

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DOI - Digital Object Identifier

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Jazyk výsledku

angličtina

Název v původním jazyce

NLTE models of line-driven stellar winds III. Influence of X-ray radiation on wind structure of O stars

Popis výsledku v původním jazyce

We study the influence of X rays on the wind structure of selected O stars. For this purpose we use our non local thermodynamic equilibrium (NLTE) wind code with inclusion of additional artificial source of X rays, assumed to originate in the wind shocks. We show that the influence of shock X ray emission on wind mass loss rate is relatively small. Wind terminal velocity may be slightly influenced by the presence of strong X ray sources, especially for stars cooler than Teff 35 000 K . We discuss the origin of the Lx/L 10 7 relation. For stars with thick wind this relation can be explained assuming that the cooling time depends on wind density. Stars with optically thin winds exhibiting the weak wind problem display enhanced X ray emission which may beconnected with large shock cooling length. We propose that this effect can explain the weak wind problem. Inclusion of X rays leads to a better agreement of the model ionization structure with observations.

Název v anglickém jazyce

NLTE models of line-driven stellar winds III. Influence of X-ray radiation on wind structure of O stars

Popis výsledku anglicky

We study the influence of X rays on the wind structure of selected O stars. For this purpose we use our non local thermodynamic equilibrium (NLTE) wind code with inclusion of additional artificial source of X rays, assumed to originate in the wind shocks. We show that the influence of shock X ray emission on wind mass loss rate is relatively small. Wind terminal velocity may be slightly influenced by the presence of strong X ray sources, especially for stars cooler than Teff 35 000 K . We discuss the origin of the Lx/L 10 7 relation. For stars with thick wind this relation can be explained assuming that the cooling time depends on wind density. Stars with optically thin winds exhibiting the weak wind problem display enhanced X ray emission which may beconnected with large shock cooling length. We propose that this effect can explain the weak wind problem. Inclusion of X rays leads to a better agreement of the model ionization structure with observations.

Druh

J_x - Nezařazeno - Článek v odborném periodiku (Jimp, Jsc a Jost)

CEP obor

BN - Astronomie a nebeská mechanika, astrofyzika

OECD FORD obor

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Projekt

Výsledek vznikl pri realizaci vícero projektů. Více informací v záložce Projekty.

Návaznosti

S - Specificky vyzkum na vysokych skolach

Rok uplatnění

2009

Kód důvěrnosti údajů

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

Název periodika

Monthly Notices of the Royal Astronomical Society

ISSN

0035-8711

e-ISSN

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Svazek periodika

394

Číslo periodika v rámci svazku

4

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

15

Strana od-do

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Kód UT WoS článku

000266549600029

EID výsledku v databázi Scopus

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