Predictions of the effect of clumping on the wind properties of O-type stars

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216224%3A14310%2F11%3A00049668" target="_blank" >RIV/00216224:14310/11:00049668 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/67985815:_____/11:00368890

Výsledek na webu

<a href="http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361/201014290&Itemid=129" target="_blank" >http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361/201014290&Itemid=129</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/201014290" target="_blank" >10.1051/0004-6361/201014290</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Predictions of the effect of clumping on the wind properties of O-type stars

Popis výsledku v původním jazyce

Aims. Both empirical evidence and theoretical ndings indicate that the stellar winds of massive early-type stars are inhomogeneous, i.e., porous and clumpy. For relatively dense winds, empirically derived mass-loss rates might be reconciled with predictions if these empirical rates are corrected for clumping. The predictions, however, do not account for structure in the wind. To allow for a consistent comparison, we investigate and quantify the e ect of clumpiness and porosity of the out ow on the predicted wind energy and the maximal e ect on the mass-loss rate of O-type stars. Methods. Combining non-LTE model atmospheres and a Monte Carlo method to compute the transfer of momentum from the photons to the gas, the e ect of clumping and porosity on theenergy transferred from the radiation eld to the wind is computed in out ows in which the clumping and porosity strati cation is parameterized by heuristic prescriptions. Results.

Název v anglickém jazyce

Predictions of the effect of clumping on the wind properties of O-type stars

Popis výsledku anglicky

Aims. Both empirical evidence and theoretical ndings indicate that the stellar winds of massive early-type stars are inhomogeneous, i.e., porous and clumpy. For relatively dense winds, empirically derived mass-loss rates might be reconciled with predictions if these empirical rates are corrected for clumping. The predictions, however, do not account for structure in the wind. To allow for a consistent comparison, we investigate and quantify the e ect of clumpiness and porosity of the out ow on the predicted wind energy and the maximal e ect on the mass-loss rate of O-type stars. Methods. Combining non-LTE model atmospheres and a Monte Carlo method to compute the transfer of momentum from the photons to the gas, the e ect of clumping and porosity on theenergy transferred from the radiation eld to the wind is computed in out ows in which the clumping and porosity strati cation is parameterized by heuristic prescriptions. Results.

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

<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 periodika

Astronomy and Astrophysics

ISSN

0004-6361

e-ISSN

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Svazek periodika

526

Číslo periodika v rámci svazku

—

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

11

Strana od-do

"A32"-"1"-"A32"-"11"

Kód UT WoS článku

000286458400044

EID výsledku v databázi Scopus

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