Simulations of pre-supernova feedback in spherical clouds
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F23%3A00571480" target="_blank" >RIV/67985815:_____/23:00571480 - isvavai.cz</a>
Result on the web
<a href="https://doi.org/10.1093/mnras/stad822" target="_blank" >https://doi.org/10.1093/mnras/stad822</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1093/mnras/stad822" target="_blank" >10.1093/mnras/stad822</a>
Alternative languages
Result language
angličtina
Original language name
Simulations of pre-supernova feedback in spherical clouds
Original language description
We present a 1D radiation-hydrodynamic model of a spherically symmetric cloud evolving under the influence of the self-gravity and the feedback from a star cluster forming in its centre. On one hand, the model is simple due to its 1D geometry, on the other hand, the feedback includes the ionizing radiation, stellar winds and the radiation pressure acting on gas and dust. The star cluster is formed from the gas flowing into the cloud centre and the feedback parameters are determined from stellar evolution models and the cluster star forming history. The model is compared to the semi-analytic code WARPFIELD implementing similar physical processes and exploring the scenario that the young cluster R136 in the Large Magellanic Cloud was formed due to re-collapse of the shell formed by the previous generation star cluster. A good qualitative agreement is found, however, 3-4 times higher stellar mass is needed to disrupt the cloud in our model, because it takes into account (contrary to WARPFIELD) self-gravity of the cloud surrounding the shell. We use the model to explore star formation in clouds with different mass, radius and density profile measuring their star formation efficiency (SFE), i.e. the fraction of the cloud mass converted to stars. We found that SFE is a function of a single parameter, log(SFE) alpha- n(-0.46) (hm), with n hm being the cloud mean particle density within its half-mass radius. Furthermore, we found that the feedback efficiency, i.e. a fraction of the feedback energy retained by gas, has a nearly constant value similar to 10(-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
<a href="/en/project/GA19-15008S" target="_blank" >GA19-15008S: Star formation efficiency in massive star clusters</a><br>
Continuities
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace
Others
Publication year
2023
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
1365-2966
Volume of the periodical
521
Issue of the periodical within the volume
4
Country of publishing house
US - UNITED STATES
Number of pages
13
Pages from-to
5686-5698
UT code for WoS article
000965008600005
EID of the result in the Scopus database
2-s2.0-85159861823