How fast do young star clusters expel their natal gas? Estimating the upper limit of the gas expulsion time-scale

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F20%3A10423269" target="_blank" >RIV/00216208:11320/20:10423269 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=pi-LRO8FqG" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=pi-LRO8FqG</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/staa2560" target="_blank" >10.1093/mnras/staa2560</a>

Jazyk výsledku

angličtina

Název v původním jazyce

How fast do young star clusters expel their natal gas? Estimating the upper limit of the gas expulsion time-scale

Popis výsledku v původním jazyce

Formation of massive stars within embedded star clusters starts a complex interplay between their feedback, inflowing gas, and stellar dynamics, which often includes close stellar encounters. Hydrodynamical simulations usually resort to substantial simplifications to model embedded clusters. Here, we address the simplification which approximates the whole star cluster by a single sink particle, which completely neglects the internal stellar dynamics. In order to model the internal stellar dynamics, we implement a Hermite predictor-corrector integration scheme to the hydrodynamic code FLASH. As we illustrate by a suite of tests, this integrator significantly outperforms the current leap-frog scheme, and it is able to follow the dynamics of small compact stellar systems without the necessity to soften the gravitational potential. We find that resolving individual massive stars instead of representing the whole cluster by a single energetic source has a profound influence on the gas component: for clusters of mass less than approximate to 3 x 10(3)M(circle dot), it slows gas expulsion by a factor of approximate to 5 to approximate to 1Myr, and it results in substantially more complex gas structures. With increasing cluster mass (up to approximate to 3 x 10(3)M(circle dot)), the gas expulsion time-scale slightly decreases. However, more massive clusters (greater than or similar to 5 x 10(3)M(circle dot)) are unable to clear their natal gas with photoionizing radiation and stellar winds only if they form with a star formation efficiency (SFE) of 1/3. This implies that the more massive clusters are either cleared with another feedback mechanism or they form with an SFE higher than 1/3.

Název v anglickém jazyce

How fast do young star clusters expel their natal gas? Estimating the upper limit of the gas expulsion time-scale

Popis výsledku anglicky

Formation of massive stars within embedded star clusters starts a complex interplay between their feedback, inflowing gas, and stellar dynamics, which often includes close stellar encounters. Hydrodynamical simulations usually resort to substantial simplifications to model embedded clusters. Here, we address the simplification which approximates the whole star cluster by a single sink particle, which completely neglects the internal stellar dynamics. In order to model the internal stellar dynamics, we implement a Hermite predictor-corrector integration scheme to the hydrodynamic code FLASH. As we illustrate by a suite of tests, this integrator significantly outperforms the current leap-frog scheme, and it is able to follow the dynamics of small compact stellar systems without the necessity to soften the gravitational potential. We find that resolving individual massive stars instead of representing the whole cluster by a single energetic source has a profound influence on the gas component: for clusters of mass less than approximate to 3 x 10(3)M(circle dot), it slows gas expulsion by a factor of approximate to 5 to approximate to 1Myr, and it results in substantially more complex gas structures. With increasing cluster mass (up to approximate to 3 x 10(3)M(circle dot)), the gas expulsion time-scale slightly decreases. However, more massive clusters (greater than or similar to 5 x 10(3)M(circle dot)) are unable to clear their natal gas with photoionizing radiation and stellar winds only if they form with a star formation efficiency (SFE) of 1/3. This implies that the more massive clusters are either cleared with another feedback mechanism or they form with an SFE higher than 1/3.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2020

Kód důvěrnosti údajů

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

Název periodika

Monthly Notices of the Royal Astronomical Society

ISSN

0035-8711

e-ISSN

—

Svazek periodika

499

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

20

Strana od-do

748-767

Kód UT WoS článku

000587761200055

EID výsledku v databázi Scopus

2-s2.0-85098562734