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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

  • Czech description

Classification

  • Type

    J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database

  • CEP classification

  • 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