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
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: |
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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: |
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URI: | http://kups.ub.uni-koeln.de/id/eprint/68277 |
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