Comoving frame models of hot star winds II. Reduction of O star wind mass-loss rates in global models

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F17%3A00482625" target="_blank" >RIV/67985815:_____/17:00482625 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/00216224:14310/17:00095040

Výsledek na webu

<a href="http://dx.doi.org/10.1051/0004-6361/201730723" target="_blank" >http://dx.doi.org/10.1051/0004-6361/201730723</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/201730723" target="_blank" >10.1051/0004-6361/201730723</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Comoving frame models of hot star winds II. Reduction of O star wind mass-loss rates in global models

Popis výsledku v původním jazyce

We calculate global (unified) wind models of main-sequence, giant, and supergiant O stars from our Galaxy. The models are calculated by solving hydrodynamic, kinetic equilibrium (also known as NLTE) and comoving frame (CMF) radiative transfer equations from the (nearly) hydrostatic photosphere to the supersonic wind. For given stellar parameters, our models predict the photosphere and wind structure and in particular the wind mass-loss rates without any free parameters. Our predicted mass-loss rates are by a factor of 2-5 lower than the commonly used predictions. A possible cause of the difference is abandoning of the Sobolev approximation for the calculation of the radiative force, because our models agree with predictions of CMF NLTE radiative transfer codes. Our predicted mass-loss rates agree nicely with the mass-loss rates derived from observed near-infrared and X-ray line profiles and are slightly lower than mass-loss rates derived from combined UV and H alpha diagnostics.

Název v anglickém jazyce

Comoving frame models of hot star winds II. Reduction of O star wind mass-loss rates in global models

Popis výsledku anglicky

We calculate global (unified) wind models of main-sequence, giant, and supergiant O stars from our Galaxy. The models are calculated by solving hydrodynamic, kinetic equilibrium (also known as NLTE) and comoving frame (CMF) radiative transfer equations from the (nearly) hydrostatic photosphere to the supersonic wind. For given stellar parameters, our models predict the photosphere and wind structure and in particular the wind mass-loss rates without any free parameters. Our predicted mass-loss rates are by a factor of 2-5 lower than the commonly used predictions. A possible cause of the difference is abandoning of the Sobolev approximation for the calculation of the radiative force, because our models agree with predictions of CMF NLTE radiative transfer codes. Our predicted mass-loss rates agree nicely with the mass-loss rates derived from observed near-infrared and X-ray line profiles and are slightly lower than mass-loss rates derived from combined UV and H alpha diagnostics.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA13-10589S" target="_blank" >GA13-10589S: Ztráta hmoty horkých hmotných hvězd</a><br>

Návaznosti

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

Rok uplatnění

2017

Kód důvěrnosti údajů

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

Název periodika

Astronomy & Astrophysics

ISSN

1432-0746

e-ISSN

—

Svazek periodika

606

Číslo periodika v rámci svazku

October

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

12

Strana od-do

"A31/1"-"A31/12"

Kód UT WoS článku

000412876000001

EID výsledku v databázi Scopus

2-s2.0-85031826065