How fast do young star clusters expel their natal gas? Estimating the upper limit of the gas expulsion time-scale
The result's identifiers
Result code in 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>
Result on the web
<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>
Alternative languages
Result language
angličtina
Original language name
How fast do young star clusters expel their natal gas? Estimating the upper limit of the gas expulsion time-scale
Original language description
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.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
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Continuities
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace
Others
Publication year
2020
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Monthly Notices of the Royal Astronomical Society
ISSN
0035-8711
e-ISSN
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Volume of the periodical
499
Issue of the periodical within the volume
1
Country of publishing house
GB - UNITED KINGDOM
Number of pages
20
Pages from-to
748-767
UT code for WoS article
000587761200055
EID of the result in the Scopus database
2-s2.0-85098562734