Formation of Primordial Stars in a ΛCDM Universe

By Naoki Yoshida, K. Omukai, L. Hernquist, Tom Abel. 2006

388 citations recorded by the source corpus.

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Citations in the corpus

FORMATION RATES OF POPULATION III STARS AND CHEMICAL ENRICHMENT OF HALOS DURING THE REIONIZATION ERA (2009, methodology): “This expectation is based on theoretical models and numerical simulations (Abel et al. 2002; Omukai & Yoshii 2003; Yoshida et al. 2006; Gao et al. 2007), but there is some tension with the abundance patterns observed in the most metal-poor Milky Way stars, which are better explained under the…”
Galaxy formation theory (2010, background): “As such, this problem has been examined and exploredin significant detail (Abel et al. 2002; Yoshida et al. 2006; Gao et al. 2007).”
EVOLUTION OF MASSIVE PROTOSTARS WITH HIGH ACCRETION RATES (2008, background): “By coincidence, the similar high accretion rates are expected for protostars forming in the early universe (e.g., Omukai & Nishi 1998; Yoshida et al. 2006).”
The First Billion Years project: the escape fraction of ionizing photons in the epoch of reionization (2015, methodology): “For the FiBY simulations, we have added a full non-equilibrium primordial chemistry network (Abel et al. 1997; Galli & Palla 1998; Yoshida et al. 2006) including molecular cooling functions for H2 and HD.”
Direct Cosmological Simulations of the Growth of Black Holes and Galaxies (2007, background): “…black hole ofmass 104Y106M (Carr &Rees 1984; Bromm& Loeb 2003; Begelman et al. 2006) or, (2) alternatively, smaller black hole seeds (M 102 M ) may form from the first Popu- lation III stars at z 30 and grow exponentially from then on (Abel et al. 2002; Bromm & Larson 2004; Yoshida et al. 2006).”
Population III Star Formation in a ΛCDM Universe. II. Effects of a Photodissociating Background (2007, result): “…of the formation of Population III stars in a cosmological context via high-resolution simulations is becoming a mature discipline, with multiple groups finding similar results (Bromm et al. 2002; Bromm & Loeb 2004; Abel et al. 2002; O’Shea & Norman 2007; Yoshida et al. 2006b; Gao et al. 2006).”
The First Billion Years project: the impact of stellar radiation on the co-evolution of Populations II and III (2012, methodology): “For the FiBY project, we have furthermore implemented a full non-equilibrium primordial chemistry network and molecular cooling functions for both H2 and HD, following Abel et al. (1997), Galli & Palla (1998), Yoshida et al. (2006), and Maio et al. (2007).”
THE MASS SPECTRUM OF THE FIRST STARS (2014, result): “First, the internal properties of our samples are similar to those in previous studies (Yoshida et al. 2006; O’Shea & Norman 2007; Hirano et al. 2014).”
The First Stars (2012, methodology): “An alternative approach was introduced by Yoshida et al. (2006).”
The Formation of the First Stars. II. Radiative Feedback Processes and Implications for the Initial Mass Function (2007, background): “In the absence of any elements heavier than helium (other than trace amounts of lithium) the chemistry and thermodynamics of the gas are very simple (Abel et al. 2002, hereafter ABN02; Bromm et al. 2002).”
Formation and evolution of primordial protostellar systems (2012, background): “The gas cloud then becomes Jeans unstable and undergoes runaway collapse, resulting in the formation of a protostar at the centre of the halo (Yoshida et al. 2006; Yoshida, Omukai & Hernquist 2008).”
The First Stars: Mass Growth Under Protostellar Feedback (2011, methodology): “We furthermore found that the angular momentum profile of the minihalo gas immediately before initial sink formation was very similar to the cosmological simulations of Abel et al. (2002) and Yoshida et al. (2006), despite their lower values of σ8 (0.7 and 0.9, respectively).”
A case study of hurdle and generalized additive models in astronomy: the escape of ionizing radiation (2018, methodology): “The FiBY simulations included an additional full non-equilibrium primordial chemistry network (Abel et al. 1997; Yoshida et al. 2006; Maio et al. 2011; Johnson, Dalla Vecchia & Khochfar 2013) with molecular cooling functions for H2 and HD, a thermal SN II feedback model (Dalla Vecchia & Schaye…”
SIMULATIONS ON A MOVING MESH: THE CLUSTERED FORMATION OF POPULATION III PROTOSTARS (2011, methodology): “…are in local thermodynamic equilibrium, and write the escape probabilities for the various transitions as βesc,ul = 1− exp(−τul) τul , (3) where we use the approximation that τul ≃ αulLs , (4) where αul is the line absorption coefficient and Ls is the Sobolev length (Yoshida et al. 2006).”
The first galaxies : assembly, cooling and the onset of turbulence (2008, background): “While turbulence does not seem to play a role in minihaloes, at least on scales comparable to their virial radius (Yoshida et al. 2006), turbulent motions could become important in more massive haloes, where accretion of cold gas from filaments in combination with a softened equation of state…”
Probing the formation of the first low‐mass stars with stellar archaeology (2007, background): “…widely believed that these first stars were very massive; numerical simulations show that the collapse and fragmentation of primordial gas, where cooling relies on molecular hydrogen only, leads to Pop III stars with masses > 100M⊙ (e.g. Abel et al. 2002; Bromm et al. 2002; Yoshida et al. 2006).”
Formation of supermassive black holes (2010, background): “Simulations of the collapse of primordial molecular clouds (Bromm et al, 1999, 2002; Abel et al, 2000; Yoshida et al, 2006; Gao et al, 2007) suggest that the first generation of stars contained many ‘very massive stars’ (VMSs) with m?”
Uncertainties in H2 and HD chemistry and cooling and their role in early structure formation (2008, background): “…view see Clark, Glover & E-mail: sglover@aip.de Klessen 2008), and since the high gas temperature leads to a high protostellar accretion rate, there seems little to limit the growth of the first stars, which may easily grow to ∼100 M or more (see e.g. Yoshida et al. 2006; O’Shea & Norman 2007).”