Mass loss in main-sequence B stars

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216224%3A14310%2F14%3A00073773" target="_blank" >RIV/00216224:14310/14:00073773 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1051/0004-6361/20131980" target="_blank" >http://dx.doi.org/10.1051/0004-6361/20131980</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/20131980" target="_blank" >10.1051/0004-6361/20131980</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Mass loss in main-sequence B stars

Popis výsledku v původním jazyce

We calculate radiatively driven wind models of main-sequence B stars and provide the wind mass-loss rates and terminal velocities. The main-sequence mass-loss rate strongly depends on the stellar effective temperature. For the hottest B stars the mass-loss rate amounts to 1d-9 Mo/year, while for the cooler ones the mass-loss rate is lower by more than three orders of magnitude. Main-sequence B stars with solar abundance and effective temperatures lower than about 15000 K (later than spectral type B5) donot have any homogeneous line-driven wind. We predict the wind mass-loss rates for the solar chemical composition and for the modified abundance of heavier elements to study the winds of chemically peculiar stars. The mass-loss rate may either increaseor decrease with increasing abundance, depending on the importance of the induced emergent flux redistribution. Stars with overabundant silicon may have homogeneous winds even below the solar abundance wind limit at 15000 K.

Název v anglickém jazyce

Mass loss in main-sequence B stars

Popis výsledku anglicky

We calculate radiatively driven wind models of main-sequence B stars and provide the wind mass-loss rates and terminal velocities. The main-sequence mass-loss rate strongly depends on the stellar effective temperature. For the hottest B stars the mass-loss rate amounts to 1d-9 Mo/year, while for the cooler ones the mass-loss rate is lower by more than three orders of magnitude. Main-sequence B stars with solar abundance and effective temperatures lower than about 15000 K (later than spectral type B5) donot have any homogeneous line-driven wind. We predict the wind mass-loss rates for the solar chemical composition and for the modified abundance of heavier elements to study the winds of chemically peculiar stars. The mass-loss rate may either increaseor decrease with increasing abundance, depending on the importance of the induced emergent flux redistribution. Stars with overabundant silicon may have homogeneous winds even below the solar abundance wind limit at 15000 K.

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/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

2014

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

564

Číslo periodika v rámci svazku

april

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

10

Strana od-do

"A70-1"-"A70-10"

Kód UT WoS článku

000334671000070

EID výsledku v databázi Scopus

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