Feedback and star formation efficiency in high-mass star-forming regions
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F25%3A00642471" target="_blank" >RIV/67985815:_____/25:00642471 - isvavai.cz</a>
Result on the web
<a href="https://hdl.handle.net/11104/0372436" target="_blank" >https://hdl.handle.net/11104/0372436</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1093/mnras/staf1868" target="_blank" >10.1093/mnras/staf1868</a>
Alternative languages
Result language
angličtina
Original language name
Feedback and star formation efficiency in high-mass star-forming regions
Original language description
To advance our understanding of massive star formation, it is essential to perform a comprehensive suite of simulations that explore the relevant parameter space and include enough physics to enable a comparison with observational data. We simulate the gravitational collapse of isolated parsec-scale turbulent cores using the flash code, modelling stars as sink particles. Our simulations incorporate ionizing radiation and the associated radiation pressure from stellar sources, and non-ionizing radiation and its dust heating, along with self-consistent chemistry, to capture the properties of emerging ultra-compact H ii regions. Dust, gas, and radiation temperature are computed independently. The initial conditions are informed by ALMAGAL observations. We assess stellar feedback, comparing ionizing radiation and radiation pressure. Ionizing radiation ultimately halts mass accretion onto sink particles, while direct radiation pressure enhances the expansion of H ii regions. Heating from non-ionizing radiation suppresses fragmentation. We examine the effect of spatial resolution, finding that higher resolution leads to more sink particles, which are situated in environments with higher densities. As a result, ionizing radiation remains trapped longer, allowing continued accretion and yielding a higher overall star formation efficiency (SFE). We explore the impact of varying initial conditions, including the core density profile, virial parameter, and metallicity. Our parameter study reveals that a flatter density profile, higher virial parameter, and increased metallicity promote fragmentation, potentially enhancing the SFE by slowing the growth of the most massive stars and delaying the onset of stellar feedback. Overall, we find SFEs between 35 per cent and 57 per cent. Stellar feedback dictates the final SFE.
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
2025
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
544
Issue of the periodical within the volume
2
Country of publishing house
US - UNITED STATES
Number of pages
24
Pages from-to
2136-2159
UT code for WoS article
001617345300001
EID of the result in the Scopus database
2-s2.0-105022020216