X-ray emission from hydrodynamical wind simulations in non-LTE models

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216224%3A14310%2F11%3A00050049" target="_blank" >RIV/00216224:14310/11:00050049 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/67985815:_____/11:00372640

Výsledek na webu

<a href="http://adsabs.harvard.edu/abs/2011IAUS..272..614K" target="_blank" >http://adsabs.harvard.edu/abs/2011IAUS..272..614K</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1017/S1743921311011562" target="_blank" >10.1017/S1743921311011562</a>

Jazyk výsledku

angličtina

Název v původním jazyce

X-ray emission from hydrodynamical wind simulations in non-LTE models

Popis výsledku v původním jazyce

Massive hot stars are strong sources of X-ray emission originating in their winds. Although hydrodynamical wind simulations that are able to predict this X-ray emission are available, the inclusion of X-rays in stationary wind models is usually based oncrude approximations. To improve this, we use results from time-dependent hydrodynamical simulations of the line-driven wind instability to derive an analytical approximation of X-ray emission in the stellar wind. We use this approximation in our non-LTEwind models and find that an improved inclusion of X-rays leads to a better agreement between model ionization fractions and those derived from observations. Furthermore, the slope of the Lx-L relation is in better agreement with observations, albeit the X-ray luminosity is underestimated by a factor of three. We propose that a possible solution for this discrepancy is connected with the wind porosity.

Název v anglickém jazyce

X-ray emission from hydrodynamical wind simulations in non-LTE models

Popis výsledku anglicky

Massive hot stars are strong sources of X-ray emission originating in their winds. Although hydrodynamical wind simulations that are able to predict this X-ray emission are available, the inclusion of X-rays in stationary wind models is usually based oncrude approximations. To improve this, we use results from time-dependent hydrodynamical simulations of the line-driven wind instability to derive an analytical approximation of X-ray emission in the stellar wind. We use this approximation in our non-LTEwind models and find that an improved inclusion of X-rays leads to a better agreement between model ionization fractions and those derived from observations. Furthermore, the slope of the Lx-L relation is in better agreement with observations, albeit the X-ray luminosity is underestimated by a factor of three. We propose that a possible solution for this discrepancy is connected with the wind porosity.

Druh

D - Stať ve sborníku

CEP obor

BN - Astronomie a nebeská mechanika, astrofyzika

OECD FORD obor

—

Projekt

<a href="/cs/project/GA205%2F08%2F0003" target="_blank" >GA205/08/0003: Předpovědi rychlosti ztráty hmoty horkých hvězd</a><br>

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Rok uplatnění

2011

Kód důvěrnosti údajů

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

Název statě ve sborníku

Active OB stars: structure, evolution, mass loss, and critical limits

ISBN

978-0-521-19840-0

ISSN

—

e-ISSN

—

Počet stran výsledku

2

Strana od-do

614-615

Název nakladatele

Cambridge University Press

Místo vydání

Cambridge

Místo konání akce

Paříž, Francie

Datum konání akce

1. 1. 2010

Typ akce podle státní příslušnosti

WRD - Celosvětová akce

Kód UT WoS článku

000294438200166