Young Stellar Clusters with a Schuster Mass Distribution. I. Stationary Winds

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F13%3A00423330" target="_blank" >RIV/67985815:_____/13:00423330 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1088/0004-637X/772/2/128" target="_blank" >http://dx.doi.org/10.1088/0004-637X/772/2/128</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1088/0004-637X/772/2/128" target="_blank" >10.1088/0004-637X/772/2/128</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Young Stellar Clusters with a Schuster Mass Distribution. I. Stationary Winds

Popis výsledku v původním jazyce

Hydrodynamic models for spherically symmetric winds driven by young stellar clusters with a generalized Schuster stellar density profile are explored. For this we use both semi-analytic models and one-dimensional numerical simulations. We determine the properties of quasi-adiabatic and radiative stationary winds and define the radius at which the flow turns from subsonic to supersonic for all stellar density distributions. Strongly radiative winds significantly diminish their terminal speed and thus their mechanical luminosity is strongly reduced. This also reduces their potential negative feedback into their host galaxy interstellar medium. The critical luminosity above which radiative cooling becomes dominant within the clusters, leading to thermal instabilities which make the winds non-stationary, is determined, and its dependence on the star cluster density profile, core radius, and half-mass radius is discussed.

Název v anglickém jazyce

Young Stellar Clusters with a Schuster Mass Distribution. I. Stationary Winds

Popis výsledku anglicky

Hydrodynamic models for spherically symmetric winds driven by young stellar clusters with a generalized Schuster stellar density profile are explored. For this we use both semi-analytic models and one-dimensional numerical simulations. We determine the properties of quasi-adiabatic and radiative stationary winds and define the radius at which the flow turns from subsonic to supersonic for all stellar density distributions. Strongly radiative winds significantly diminish their terminal speed and thus their mechanical luminosity is strongly reduced. This also reduces their potential negative feedback into their host galaxy interstellar medium. The critical luminosity above which radiative cooling becomes dominant within the clusters, leading to thermal instabilities which make the winds non-stationary, is determined, and its dependence on the star cluster density profile, core radius, and half-mass radius is discussed.

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/GAP209%2F12%2F1795" target="_blank" >GAP209/12/1795: Tvorba hvězd aktivovaná expandujícími obálkami</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2013

Kód důvěrnosti údajů

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

Název periodika

Astrophysical Journal

ISSN

0004-637X

e-ISSN

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Svazek periodika

772

Číslo periodika v rámci svazku

2

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

9

Strana od-do

"128/1"-"128/9"

Kód UT WoS článku

000322024700050

EID výsledku v databázi Scopus

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