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Title: 3D Radiation-hydrodynamic Simulations Resolving Interior of Rapidly Accreting Primordial Protostar
Authors: Kimura, Kazutaka
Hosokawa, Takashi  kyouindb  KAKEN_id  orcid (unconfirmed)
Sugimura, Kazuyuki
Fukushima, Hajime
Author's alias: 木村, 和貴
細川, 隆史
杉村, 和幸
Keywords: Star formation
Early universe
Supermassive black holes
Issue Date: 20-Jun-2023
Publisher: American Astronomical Society
Journal title: The Astrophysical Journal
Volume: 950
Issue: 2
Thesis number: 184
Abstract: Direct collapse of supermassive stars is a possible pathway to form supermassive black hole seeds at high redshifts. Whereas previous three-dimensional (3D) simulations demonstrate that supermassive stars form via rapid mass accretion, those resolving the stellar interior have been limited. Here, we report 3D radiation-hydrodynamic (RHD) simulations following the evolution of rapidly accreting protostars resolving the stellar interior. We use an adaptive mesh refinement code with our newly developed RHD solver employing an explicit M1 closure method. We follow the early evolution until the stellar mass reaches ∼10 M⊙ from two different initial configurations of spherical and turbulent clouds. We demonstrate that, in both cases, a swollen protostar whose radius is 100–1000 R⊙ appears, as predicted by the stellar evolution calculations. Its effective temperature remains a few thousand Kelvin, and the radiative feedback by ionizing photons is too weak to disturb the accretion flow up to the epoch examined in this work. In the turbulent case, the protostar rotates rapidly at more than 0.4 times the Keplerian velocity owing to the angular momentum provided by the initial turbulence. The protostar approximates an oblate spheroid, and its equatorial radius is more than twice the polar radius. Our results suggest that we need to consider the rapid stellar rotation to elucidate the realistic 3D protostellar evolution in the supermassive star formation.
Rights: © 2023. The Author(s). Published by the American Astronomical Society.
Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.
DOI(Published Version): 10.3847/1538-4357/acda8e
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