Formation of the First Stars by Accretion

By K. Omukai, F. Palla. 2003

246 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/a52d3af1906c413f2130aec385e2d73ac9db5cc7

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In Astronomy and Astrophysics

Citations in the corpus

Radiation Hydrodynamic Evolution of Primordial H II Regions (2003, background): “However, see Omukai & Palla (2003) and Omukai & Inutsuka (2002) for a markedly different view.”
Resolving the Formation of Protogalaxies. I. Virialization (2007, background): “They are believed to have stellar masses ∼100 M⊙ (Abel et al. 2002; Omukai & Palla 2003; Tan & McKee 2004; Yoshida et al. 2006b) and produce ∼1050 photons s−1 that can ionize hydrogen and dissociate H2 (Schaerer 2002).”
The First Stars (2003, background): “The dramatic expansion in radius, which according to Omukai & Palla (2003) would shut off further accretion, could therefore be avoided.”
The first galaxies : assembly, cooling and the onset of turbulence (2008, background): “…on to the protostellar core and imply that the first stars were predomi- ⋆ E-mail: tgreif@ita.uni-heidelberg.de nantly very massive, with M∗ & 100 M⊙ (Omukai & Palla 2003; Bromm & Loeb 2004; O’Shea & Norman 2007; but see Tan & McKee 2004; Ripamonti 2007; McKee & Tan 2007; McGreer & Bryan 2008).”
ONE HUNDRED FIRST STARS: PROTOSTELLAR EVOLUTION AND THE FINAL MASSES (2013, methodology): “(5) Note that ˙MP2 given by this equation is a function of Mstar, but its dependence is weak (Omukai & Palla 2003).”
The First Stars (2012, methodology): “In the zero angular momentum case, Tan & McKee (2004) show that they successfully reproduce the previous results of Stahler, Palla & Salpeter (1986a) and Omukai & Palla (2001, 2003).”
Simulations of Early Structure Formation: Primordial Gas Clouds (2003, methodology): “…stars, the luminosity per unit stellar mass is L(ν) ≈ 3× 1021 erg s−1 Hz−1 M−1⊙ in the Lyman-Werner band, with only a weak dependence on the stellar mass. Omukai & Palla (2003) argue that Population III stars with masses up to 600 M⊙ could form by rapid accretion, whereas Abel et al. (2002)…”
FORMATION OF PRIMORDIAL SUPERMASSIVE STARS BY RAPID MASS ACCRETION (2013, methodology): “Recent theoretical work investigates how massive such primordial stars are, studying the late evolutionary stage whereby a protostar grows in mass via mass accretion from a surrounding envelope (e.g., 1 Department of Physics and Research Center for the Early Universe, The University of Tokyo, Tokyo ”
The Cosmic Dispersion Measure from Gamma-Ray Burst Afterglows: Probing the Reionization History and the Burst Environment (2003, background): “The first generation stars could be very massive (Abel, Bryan, & Norman 2002; Bromm, Coppi, & Larson 2002; Omukai & Palla 2003), so that they may end as brighter GRBs.”
Early Cosmological H II/He III Regions and Their Impact on Second-Generation Star Formation (2006, background): “Following the argument of Omukai & Palla (2003) and Yoshida et al. (2006), we expect the central protostar in this buried H ii region will grow, to be a massive metal-free star.”
Supermassive black hole formation by direct collapse: keeping protogalactic gas H2 free in dark matter haloes with virial temperatures Tvir > rsim 104 K (2009, background): “…does not have the time to be incorporated onto the proto–star before it settles to the zero–age main sequence (ZAMS); conversely, the mass inside this radius will accrete onto the protostar before the star settles to the ZAMS (e.g. Abel et al. 2002; Omukai & Palla 2003; O’Shea & Norman 2007).”
Fragmentation of star-forming clouds enriched with the first dust (2006, background): “Unfortunately, both the mass range and the shape of the IMF are still hampered from our limited understanding of the accretion physics and protostellar feedback effects (Omukai & Palla 2003; Bromm & Loeb 2004; Tan & McKee 2004; see also Bromm & Larson 2004 for a thorough review).”
EVOLUTION OF MASSIVE PROTOSTARS VIA DISK ACCRETION (2010, methodology): “Protostellar evolution with high accretion rates has been studied with zero or very low metallicities under the assumption of spherically symmetric accretion (e.g., Stahler, Palla & Salpeter 1986; Omukai & Palla 2001, 2003; Hosokawa & Omukai 2009b).”
Population III Star Formation in a ΛCDM Universe. I. The Effect of Formation Redshift and Environment on Protostellar Accretion Rate (2006, background): “As discussed by Omukai & Palla (2003) and Tan & McKee (2004), radiative feedback from the evolving protostar will strongly affect the dynamics of the accreting gas.”
Titans of the early Universe: The Prato statement on the origin of the first supermassive black holes (2018, background): “Unable to cool to thermal equilibrium, these stars dramatically expand before reaching the main sequence (Omukai & Palla 2001, 2003).”
Population III Star Formation in a ΛCDM Universe. II. Effects of a Photodissociating Background (2007, background): “For example, Omukai & Palla (2003) suggest that an increase in accretion rate above ṁ ’ 4 ;10 3 M yr 1 will actually result in a decrease in the final mass of the star due to radiative feedback from the evolving protostar.”
Can Supermassive Black Holes Form in Metal-enriched High-Redshift Protogalaxies? (2008, background): “During the accretion phase, radiative and mechanical feedback effects might become important and eventually halt the accretion at some phase (e.g., Omukai & Palla 2003; McKee & Tan 2008).”
The First Billion Years project: the impact of stellar radiation on the co-evolution of Populations II and III (2012, methodology): “We choose M∗,upper = 500 M⊙, as the former authors show that this is roughly the maximum mass that is likely attainable for Pop III stars under typical conditions (see also Omukai & Palla 2001, 2003).”