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Toward Understanding Massive Star Formation
AbstractAlthough fundamental for astrophysics, the processes that produce massive stars are not well understood. Large distances, high extinction, and short timescales of critical evolutionary phases
Formation of Primordial Supermassive Stars by Rapid Mass Accretion
Supermassive stars (SMSs) forming via very rapid mass accretion (Mdot >~ 0.1 Msun/yr) could be precursors of supermassive black holes observed beyond redshift of about 6. Extending our previous work,
RAPIDLY ACCRETING SUPERGIANT PROTOSTARS: EMBRYOS OF SUPERMASSIVE BLACK HOLES?
Direct collapse of supermassive stars (SMSs) is a possible pathway for generating supermassive black holes in the early universe. It is expected that an SMS could form via very rapid mass accretion
EVOLUTION OF MASSIVE PROTOSTARS VIA DISK ACCRETION
Mass accretion onto (proto-)stars at high accretion rates M-dot{sub *}> 10{sup -4} M{sub sun} yr{sup -1} is expected in massive star formation. We study the evolution of massive protostars at such
On the Formation of Massive Stars
We calculate numerically the collapse of slowly rotating, nonmagnetic, massive molecular clumps of masses 30, 60, and 120 M☉, which conceivably could lead to the formation of massive stars. Because
One Hundred First Stars : Protostellar Evolution and the Final Masses
We perform a large set of radiation hydrodynamic simulations of primordial star formation in a fully cosmological context. Our statistical sample of 100 First Stars shows that the first generation of
Protostellar Feedback Halts the Growth of the First Stars in the Universe
TLDR
Radiation-hydrodynamics simulations suggest that most of the first stars in the universe might have been less massive than previously thought, and may help explain the fact that there are no signatures of the pair-instability supernovae in abundance patterns of metal-poor stars in the authors' galaxy.
Massive stars and the energy balance of the ISM: I. The imapct of an isolated 60 M star
We present results of numerical simulations carried out with a two-dimensional radiation hydrodynamics code in order to study the impact of massive stars on their surrounding interstellar medium.
Massive Stars and the Energy Balance of the Interstellar Medium. II. The 35 M☉ Star and a Solution to the “Missing Wind Problem”
We continue our numerical analysis of the morphological and energetic influence of massive stars on their ambient interstellar medium for a 35 M☉ star that evolves from the main-sequence through red
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