In this paper, we have studied the protostellar evolution
under very rapid accretion supposed for the DC, performing 3D
RHD simulations resolving the stellar interior structure. We
have used the AMR code SFUMATO-RT, in which we have
implemented a newly developed RHD solver employing an
explicit M1 closure method. We follow the evolution for about
10 yr after the protostar formation, during which the stellar
mass increases to ∼10 Me.
In one case starting from a spherical cloud, a swollen protostar
forms as expected by previous 1D stellar evolution calculations.
At the end of the simulation when M* ∼ 10 Me, the stellar
radius is ;1000 Re, the luminosity is ∼105 Le, and the effective
temperature is ;4000 K. Such protostars with a cool atmosphere
emit a negligible amount of ionizing photons, and the resulting
radiative feedback is too weak to disturb the accretion.
In the other case starting from a turbulent cloud, a rapidly
rotating swollen protostar appears with some different properties from the counterpart in the spherical case. The protostar
rotates at more than about 0.4 times the Keplerian velocity
everywhere in the interior due to the angular momentum
brought by the accreting gas. As a result, the equatorial radius
is more than twice as large as the polar one. Also in this case,
the effective temperature remains several thousand Kelvin and
the radiative feedback is ineffective.
We have followed the protostellar birth and subsequent
evolution for ∼10 yr expected in the DC. This is only the
beginning of the evolution until the formation of the seed BH
after approximately a megayear. Our 3D RHD simulations
have the potential to reveal the realistic protostellar evolution in
the later stage, for which only 1D modeling has been applied
so far.
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Acknowledgments
We are grateful to Tomoaki Matsumoto, Kazuyuki Omukai,
Kunihito Ioka, Ryoki Matsukoba, Shinsuke Takasao, Kengo
Tomida, and Takahiro Tanaka for fruitful discussions and
comments. The numerical simulations were carried out on
XC50 Aterui II at the Center for Computational Astrophysics (CfCA) of the National Astronomical Observatory of
Japan, and Yukawa-21 at Yukawa Institute for Theoretical
Physics of Kyoto University. This research could never be
accomplished without the support of Grants-in-Aid for
Scientific Research (T.H.: Nos. 19H01934, 21H00041; K.S.:
No. 21K20373) from the Japan Society for the Promotion of
Science. This work is also supported by JST SPRING, grant
No. JPMJSP2110 (K.K.), the ANRI Fellowship (K.K.), and the
Hakubi Project Funding of Kyoto University (K.S.).
ORCID iDs
Kazutaka Kimura https://orcid.org/0000-0001-8382-3966
Takashi Hosokawa https://orcid.org/0000-0003-3127-5982
Kazuyuki Sugimura https://orcid.org/0000-0001-7842-5488
Hajime Fukushima https://orcid.org/0000-0002-0547-3208
...
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