Universität zu Köln

Martinez-Gonzalez, Sergio ORCID: 0000-0002-4371-3823, Wunsch, Richard ORCID: 0000-0003-1848-8967, Tenorio-Tagle, Guillermo, Silich, Sergiy, Szecsi, Dorottya ORCID: 0000-0001-6473-7085 and Palous, Jan ORCID: 0000-0001-6729-2851 (2022). Dust Grain Growth and Dusty Supernovae in Low-metallicity Molecular Clouds. Astrophys. J., 934 (1). BRISTOL: IOP Publishing Ltd. ISSN 1538-4357

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Abstract

We present 3D hydrodynamical models of the evolution of superbubbles powered by stellar winds and supernovae from young coeval massive star clusters within low-metallicity (Z = 0.02 Z(circle dot)), clumpy molecular clouds. We explore the initial stages of the superbubble evolution, including the occurrence of pair-instability and core-collapse supernovae. Our aim is to study the occurrence of dust grain growth within orbiting dusty clumps, and in the superbubble's swept-up supershell. We also aim to address the survival of dust grains produced by sequential supernovae. The model accounts for the star cluster gravitational potential and self-gravity of the parent cloud. It also considers radiative cooling (including that induced by dust) and a state-of-the-art population synthesis model for the coeval cluster. As shown before, a superbubble embedded into a clumpy medium becomes highly distorted, expanding mostly due to the hot gas streaming through low-density channels Our results indicate that in the case of massive (similar to 10 M-circle dot) molecular clouds, hosting a super star cluster (similar to 5.6 x 10(5) M-circle dot), grain growth increments the dust mass at a rate similar to 4.8 x 10(-5) M-circle dot yr(-1) during the first 2.5 Myr of the superbubble's evolution, while the net contribution of pair-instability and core-collapse supernovae to the superbubble's dust budget is similar to 1200 M circle dot (M-SC/5.6 x 10(5) M-circle dot), where M-SC is the stellar mass of the starburst. Therefore, dust grain growth and dust injection by supernovae lead to the creation of, without invoking a top-heavy initial mass function, massive amounts of dust within low-metallicity star-forming molecular clouds, in accordance with the large dust mass present in galaxies soon after the onset of cosmic reionization.

Item Type:	Journal Article
Creators:	Creators Email ORCID ORCID Put Code Martinez-Gonzalez, Sergio UNSPECIFIED orcid.org/0000-0002-4371-3823 UNSPECIFIED Wunsch, Richard UNSPECIFIED orcid.org/0000-0003-1848-8967 UNSPECIFIED Tenorio-Tagle, Guillermo UNSPECIFIED UNSPECIFIED UNSPECIFIED Silich, Sergiy UNSPECIFIED UNSPECIFIED UNSPECIFIED Szecsi, Dorottya UNSPECIFIED orcid.org/0000-0001-6473-7085 UNSPECIFIED Palous, Jan UNSPECIFIED orcid.org/0000-0001-6729-2851 UNSPECIFIED
URN:	urn:nbn:de:hbz:38-682773
DOI:	10.3847/1538-4357/ac77fe
Journal or Publication Title:	Astrophys. J.
Volume:	934
Number:	1
Date:	2022
Publisher:	IOP Publishing Ltd
Place of Publication:	BRISTOL
ISSN:	1538-4357
Language:	English
Faculty:	Unspecified
Divisions:	Unspecified
Subjects:	no entry
Uncontrolled Keywords:	Keywords Language WIND-BLOWN BUBBLES; STELLAR CLUSTERS; MASS-LOSS; INTERSTELLAR DUST; O-STARS; EVOLUTION; FEEDBACK; REMNANTS; EXPLOSIONS; GALAXIES Multiple languages Astronomy & Astrophysics Multiple languages
URI:	http://kups.ub.uni-koeln.de/id/eprint/68277