Universität zu Köln

Zimmermann, Birka ORCID: 0009-0005-3040-9864, Walch, Stefanie ORCID: 0000-0001-6941-7638, Clarke, Seamus D ORCID: 0000-0001-9751-4603, Wünsch, Richard ORCID: 0000-0003-1848-8967 and Klepitko, Andre ORCID: 0000-0002-5570-1184 (2025). Feedback and star formation efficiency in high-mass star-forming regions. Monthly Notices of the Royal Astronomical Society, 544 (2). pp. 2136-2159. Oxford University Press. ISSN 0035-8711

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Abstract

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.

Item Type:	Article
Creators:	Creators Email ORCID ORCID Put Code Zimmermann, Birka UNSPECIFIED https://orcid.org/0009-0005-3040-9864 UNSPECIFIED Walch, Stefanie UNSPECIFIED https://orcid.org/0000-0001-6941-7638 UNSPECIFIED Clarke, Seamus D UNSPECIFIED https://orcid.org/0000-0001-9751-4603 UNSPECIFIED Wünsch, Richard UNSPECIFIED https://orcid.org/0000-0003-1848-8967 UNSPECIFIED Klepitko, Andre UNSPECIFIED https://orcid.org/0000-0002-5570-1184 UNSPECIFIED
URN:	urn:nbn:de:hbz:38-812145
Identification Number:	10.1093/mnras/staf1868
Journal or Publication Title:	Monthly Notices of the Royal Astronomical Society
Volume:	544
Number:	2
Page Range:	pp. 2136-2159
Number of Pages:	24
Date:	December 2025
Publisher:	Oxford University Press
ISSN:	0035-8711
Language:	English
Faculty:	Faculty of Mathematics and Natural Sciences
Divisions:	Faculty of Mathematics and Natural Sciences > Department of Physics > Institute of Physics I
Subjects:	Physics
Uncontrolled Keywords:	Keywords Language hydrodynamics ; radiative transfer ; software: simulations ; stars: formation ; stars: massive English
['eprint_fieldname_oa_funders' not defined]:	Publikationsfonds UzK
Refereed:	Yes
URI:	http://kups.ub.uni-koeln.de/id/eprint/81214