The formation of secondary stellar generations in massive young star clusters from rapidly cooling shocked stellar winds

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F17%3A00473891" target="_blank" >RIV/67985815:_____/17:00473891 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.3847/1538-4357/835/1/60" target="_blank" >http://dx.doi.org/10.3847/1538-4357/835/1/60</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/1538-4357/835/1/60" target="_blank" >10.3847/1538-4357/835/1/60</a>

Jazyk výsledku

angličtina

Název v původním jazyce

The formation of secondary stellar generations in massive young star clusters from rapidly cooling shocked stellar winds

Popis výsledku v původním jazyce

We study a model of rapidly cooling shocked stellar winds in young massive clusters and estimate the circumstances under which secondary star formation, out of the reinserted winds from a first stellar generation (1G), is possible. We have used two implementations of the model: a highly idealized, computationally inexpensive, spherically symmetric semi-analytic model, and a complex, three-dimensional radiation-hydrodynamic, simulation. The results confirm our previous findings that, in a cluster with 1G mass 10(7) M-circle dot and half-massradius 2.38 pc, the shocked stellar winds become thermally unstable, collapse into dense gaseous structures that partially accumulate inside the cluster, self-shield against ionizing stellar radiation, and form the second generation (2G) of stars. We have used the semi-analytic model to explore a subset of the parameter space covering a wide range of the observationally poorly constrained parameters: the heating efficiency, eta(he), and the mass loading, eta(ml).

Název v anglickém jazyce

The formation of secondary stellar generations in massive young star clusters from rapidly cooling shocked stellar winds

Popis výsledku anglicky

We study a model of rapidly cooling shocked stellar winds in young massive clusters and estimate the circumstances under which secondary star formation, out of the reinserted winds from a first stellar generation (1G), is possible. We have used two implementations of the model: a highly idealized, computationally inexpensive, spherically symmetric semi-analytic model, and a complex, three-dimensional radiation-hydrodynamic, simulation. The results confirm our previous findings that, in a cluster with 1G mass 10(7) M-circle dot and half-massradius 2.38 pc, the shocked stellar winds become thermally unstable, collapse into dense gaseous structures that partially accumulate inside the cluster, self-shield against ionizing stellar radiation, and form the second generation (2G) of stars. We have used the semi-analytic model to explore a subset of the parameter space covering a wide range of the observationally poorly constrained parameters: the heating efficiency, eta(he), and the mass loading, eta(ml).

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/GA15-06012S" target="_blank" >GA15-06012S: Multi-generační hvězdokupy</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

Astrophysical Journal

ISSN

0004-637X

e-ISSN

—

Svazek periodika

835

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

15

Strana od-do

"60/1"-"60/15"

Kód UT WoS článku

000393455400060

EID výsledku v databázi Scopus

2-s2.0-85011269745