Results 11 to 20 of about 17,498 (264)
The Astronomical Journal, 2022 Population III stars were the first stars to form after the Big Bang and are believed to have made the earliest contribution to the metal content of the universe beyond the products of the Big Bang nucleosynthesis.
Mikaela M. Larkin +2 more
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The mass distribution of Population III stars [PDF]
Monthly Notices of the Royal Astronomical Society, 2017 Extremely metal-poor (EMP) stars are uniquely informative on the nature of massive Population III stars. Modulo a few elements that vary with stellar evolution, the present-day photospheric abundances observed in EMP stars are representative of their natal gas cloud composition.
M. Fraser +4 more
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The Transition from Population III to Population II Stars [PDF]
The Astrophysical Journal, 2004 4 pages, 2 figures.
Fang, Taotao, Cen, Renyue
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Disc fragmentation and the formation of Population III stars [PDF]
Monthly Notices of the Royal Astronomical Society, 2015 Our understanding of population III star formation is still in its infancy. They are formed in dark matter minihalos of $\rm 10^5-10^6 M_{\odot}$ at $z=20-30$. Recent high resolution cosmological simulations show that a protostellar disk forms as a consequence of gravitational collapse and fragments into multiple clumps.
Latif, M. ~A. +1 more
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Magnetohydrodynamics of Population III Star Formation [PDF]
The Astrophysical Journal, 2008 Jet driving and fragmentation process in collapsing primordial cloud are studied using three-dimensional MHD nested grid simulations. Starting from a rotating magnetized spherical cloud with the number density of n=10^3 cm^-3, we follow the evolution of the cloud up to the stellar density n=10^22 cm^-3. We calculate 36 models parameterizing the initial
Machida, Masahiro N. +2 more
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The masses of Population III stars [PDF]
Monthly Notices of the Royal Astronomical Society, 1989 La formation de proto-etoiles de Population III est etudiee en suivant l'hypothese que la permanence des fluctuations de masse 10-1000 M○. apres l'ere de recombinaison peut etre importante dans la fragmentation des nuages massifs de masse ∼M J pour former des etoiles de population III, ou M J est la masse de Jeans pendant l'ere de ...
J. C. N. de Araujo, R. Opher
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On Population III Star Formation [PDF]
Symposium - International Astronomical Union, 1983 If primordial fluctuations were isothermal their amplitude at recombination would be non-linear on scales Mo ≃ 106÷9 M⊙. Since the Jeans mass after recombination is MJo ≃ 8 × 105 Ω−1/2 M⊙ the clouds of mass Mo would be able to form the first generation of compact objects, the so-called Population III.
A. Kashlinsky, M. J. Rees
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On the Mass of Population III Stars [PDF]
The Astrophysical Journal, 1999 Performing 1D hydrodynamical calculations coupled with non-equilibrium processes for H2 formation, we pursue the thermal and dynamical evolution of filamentary primordial clouds and attempt to make an estimate on the mass of population III stars. It is found that, almost independent of initial conditions, a filamentary cloud continues to collapse ...
Nakamura, Fumitaka, Umemura, Masayuki
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THE MOST IRON-DEFICIENT STARS AS THE POLLUTED POPULATION III STARS [PDF]
The Astrophysical Journal, 2015 Accepted for publication in ApJ ...
Yutaka Komiya +2 more
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POPULATION III STARS AROUND THE MILKY WAY [PDF]
The Astrophysical Journal, 2016 ABSTRACT We explore the possibility of observing Population III (Pop III) stars, born of primordial gas. Pop III stars with masses below 0.8 M ⊙ should survive to date though are not yet observed, but the existence of stars with low metallicity as
Yutaka Komiya +2 more
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