GRAVITATIONAL FRAGMENTATION IN TURBULENT PRIMORDIAL GAS AND THE INITIAL MASS FUNCTION OF POPULATION III STARS
نویسندگان
چکیده
منابع مشابه
Gravitational Fragmentation in Turbulent Primordial Gas and the Initial Mass Function of Population Iii Stars
We report results from numerical simulations of star formation in the early universe that focus on the dynamical behavior of metal-free gas under different initial and environmental conditions. In particular we investigate the role of turbulence, which is thought to ubiquitously accompany the collapse of high-redshift halos. We distinguish between two main cases: the birth of Population III.1 s...
متن کاملOn the Initial Mass Function of Population Iii Stars
The collapse and fragmentation of filamentary primordial gas clouds are explored using onedimensional and two-dimensional hydrodynamical simulations coupled with the nonequilibrium processes of hydrogen molecule formation. The cloud evolution is computed from the initial central density nc = 10− 10 cm. The simulations show that depending upon the initial density, there are two occasions for the...
متن کاملTowards Population III: Simulations of Primordial Gas Collapse and Fragmentation
We briefly review the motivations for studying the formation of the first “Population III” stars and present recent results from our numerical simulations in this area. We discuss the new questions raised as a result of the simulations presented by us and others at this meeting.
متن کاملNear-Critical Gravitational Collapse and the Initial Mass Function of Primordial Black Holes
The recent discovery of critical phenomena arising in gravitational collapse near the threshold of black hole formation is used to estimate the initial mass function of primordial black holes (PBHs). It is argued that the scaling relation between black hole mass and initial perturbation found for a collapsing radiation fluid in an asymptotically flat space-time also applies to PBH formation in ...
متن کاملOn the Mass of Population Iii Stars
Performing one-dimensional hydrodynamical calculations coupled with nonequilibrium processes for hydrogen molecule formation, we pursue the thermal and dynamical evolution of filamentary primordial gas clouds and attempt to make an estimate on the mass of population III stars. The cloud evolution is computed from the central proton density nc ∼ 10 2−4 cm−3 up to ∼ 1013 cm−3. It is found that, a...
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ژورنال
عنوان ژورنال: The Astrophysical Journal
سال: 2011
ISSN: 0004-637X,1538-4357
DOI: 10.1088/0004-637x/727/2/110