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Title: Disc Fragmentation and Intermittent Accretion on to Supermassive Stars
Authors: Matsukoba, R.
Vorobyov, E. I.
Sugimura, K.
Chon, S.
Hosokawa, T.
Omukai, K.
Issue Date: 2021
Publisher: Oxford University Press
Oxford University Press (OUP)
Citation: Disc Fragmentation and Intermittent Accretion on to Supermassive Stars / R. Matsukoba, E. I. Vorobyov, K. Sugimura et al. — DOI 10.18485/MS_ZMSS.2021.99.9 // Monthly Notices of the Royal Astronomical Society. — 2021. — Vol. 500. — Iss. 3. — P. 4126-4138.
Abstract: Supermassive stars (SMSs) with ∼104-105M⊙ are candidate objects for the origin of supermassive black holes observed at redshift z > 6. They are supposed to form in primordial-gas clouds that provide the central stars with gas at a high accretion rate, but their growth may be terminated in the middle due to the stellar ionizing radiation if the accretion is intermittent and its quiescent periods are longer than the Kelvin-Helmholtz (KH) time-scales at the stellar surfaces. In this paper, we examine the role of the ionizing radiation feedback based on the accretion history in two possible SMS-forming clouds extracted from cosmological simulations, following their evolution with vertically integrated two-dimensional hydrodynamic simulations with detailed thermal and chemical models. The consistent treatment of the gas thermal evolution is crucial for obtaining the realistic accretion history, as we demonstrate by performing an additional run with a barotropic equation of state, in which the fluctuation of the accretion rate is artificially suppressed. We find that although the accretion becomes intermittent due to the formation of spiral arms and clumps in gravitationally unstable discs, the quiescent periods are always shorter than the KH time-scales, implying that SMSs can form without affected by the ionizing radiation. © 2021 Oxford University Press. All rights reserved.
Access: info:eu-repo/semantics/openAccess
SCOPUS ID: 85098553854
PURE ID: 20374810
ISSN: 0035-8711
DOI: 10.18485/MS_ZMSS.2021.99.9
metadata.dc.description.sponsorship: RM acknowledges financial support from the Graduate Program on Physics for Universe of Tohoku University. EIV acknowledges support from the Austrian Science Fund (FWF) under research grant P31635-N27. KS appreciates the support by the Fellowship of the Japan Society for the Promotion of Science for Research Abroad. This work is financially supported by the Grants-in-Aid for Basic Research by the Ministry of Education, Science and Culture of Japan (SC:19J00324, TH:19H01934, KO:17H02869, 17H01102, 17H06360). The numerical simulations were carried out on XC50 at the Center for Computational Astrophysics (CfCA) of National Astronomical Observatory of Japan.
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