Populations of rotating stars II. Rapid rotators and their link to Be-type stars

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216224%3A14310%2F13%3A00067018" target="_blank" >RIV/00216224:14310/13:00067018 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1051/0004-6361/201220559" target="_blank" >http://dx.doi.org/10.1051/0004-6361/201220559</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/201220559" target="_blank" >10.1051/0004-6361/201220559</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Populations of rotating stars II. Rapid rotators and their link to Be-type stars

Popis výsledku v původním jazyce

Context. Even though it is broadly accepted that single Be stars are rapidly rotating stars surrounded by a flat rotating circumstellar disk, there is still a debate about how fast these stars rotate and also about the mechanisms involved in the angular-momentum and mass input in the disk. Aims. We study the properties of stars that rotate near their critical-rotation rate and investigate the properties of the disks formed by equatorial mass ejections. Methods. We used the most recent Geneva stellar evolutionary tracks for rapidly rotating stars that reach the critical limit and used a simple model for the disk structure. Results. We obtain that for a 9 M-circle dot star at solar metallicity, the minimum average velocity during the main-sequence (MS) phase to reach the critical velocity is around 330 km s(-1), whereas it would be 390 km s(-1) at the metallicity of the Small Magellanic Cloud (SMC).

Název v anglickém jazyce

Populations of rotating stars II. Rapid rotators and their link to Be-type stars

Popis výsledku anglicky

Context. Even though it is broadly accepted that single Be stars are rapidly rotating stars surrounded by a flat rotating circumstellar disk, there is still a debate about how fast these stars rotate and also about the mechanisms involved in the angular-momentum and mass input in the disk. Aims. We study the properties of stars that rotate near their critical-rotation rate and investigate the properties of the disks formed by equatorial mass ejections. Methods. We used the most recent Geneva stellar evolutionary tracks for rapidly rotating stars that reach the critical limit and used a simple model for the disk structure. Results. We obtain that for a 9 M-circle dot star at solar metallicity, the minimum average velocity during the main-sequence (MS) phase to reach the critical velocity is around 330 km s(-1), whereas it would be 390 km s(-1) at the metallicity of the Small Magellanic Cloud (SMC).

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

2013

Kód důvěrnosti údajů

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

Název periodika

ASTRONOMY & ASTROPHYSICS

ISSN

0004-6361

e-ISSN

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Svazek periodika

553

Číslo periodika v rámci svazku

květen

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

14

Strana od-do

"A25"-"1"-"A25"-"14"

Kód UT WoS článku

000319858700025

EID výsledku v databázi Scopus

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