Universität zu Köln

Dinnbier, Frantisek ORCID: 0000-0001-5532-4211 and Walch, Stefanie (2020). How fast do young star clusters expel their natal gas? Estimating the upper limit of the gas expulsion time-scale. Mon. Not. Roy. Astron. Soc., 499 (1). S. 748 - 768. OXFORD: OXFORD UNIV PRESS. ISSN 1365-2966

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Abstract

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.

Item Type:	Journal Article
Creators:	Creators Email ORCID ORCID Put Code Dinnbier, Frantisek UNSPECIFIED orcid.org/0000-0001-5532-4211 UNSPECIFIED Walch, Stefanie UNSPECIFIED UNSPECIFIED UNSPECIFIED
URN:	urn:nbn:de:hbz:38-313438
DOI:	10.1093/mnras/staa2560
Journal or Publication Title:	Mon. Not. Roy. Astron. Soc.
Volume:	499
Number:	1
Page Range:	S. 748 - 768
Date:	2020
Publisher:	OXFORD UNIV PRESS
Place of Publication:	OXFORD
ISSN:	1365-2966
Language:	English
Faculty:	Unspecified
Divisions:	Unspecified
Subjects:	no entry
Uncontrolled Keywords:	Keywords Language ORION-NEBULA CLUSTER; DYNAMICAL EVOLUTION; MASS SEGREGATION; IONIZING FEEDBACK; MOLECULAR CLOUDS; BINARY EVOLUTION; STELLAR FEEDBACK; SILCC PROJECT; RADIATION; CODE Multiple languages Astronomy & Astrophysics Multiple languages
URI:	http://kups.ub.uni-koeln.de/id/eprint/31343