A Radiation Hydrodynamic Model for Protostellar Collapse. II. The Second Collapse and the Birth of a Protostar

By H. Masunaga, S. Inutsuka. 2000

389 citations recorded by the source corpus.

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In Astronomy and Astrophysics

Citations in the corpus

The properties of brown dwarfs and low-mass hydrogen-burning stars formed by disc fragmentation (2008, background): “In particular it reproduces the detailed 3D results of Masunaga & Inutsuka (2000), Boss & Bodenheimer (1979), Boss & Myhill (1992), Whitehouse & Bate (2006), and also the analytic test of Spiegel (1957).”
RADIATION MAGNETOHYDRODYNAMIC SIMULATIONS OF PROTOSTELLAR COLLAPSE: NONIDEAL MAGNETOHYDRODYNAMIC EFFECTS AND EARLY FORMATION OF CIRCUMSTELLAR DISKS (2015, background): “Then the temperature quickly rises and quasi-hydrostatic objects, the first cores, are formed (Larson 1969; Masunaga & Inutsuka 2000).”
The formation mechanism of brown dwarfs (2002, background): “The gas begins to heat significantly at a density of 10213 g cm23 (Masunaga & Inutsuka 2000).”
VARIABLE PROTOSTELLAR ACCRETION WITH EPISODIC BURSTS (2015, background): “Second, we considered a stiffer equation of state taking into account the fact that the rotational and vibrational degrees of freedom of molecular hydrogen are excited only above 100 K (e.g. Masunaga & Inutsuka 2000).”
High- and Low-Velocity Magnetized Outflows in the Star Formation Process in a Gravitationally Collapsing Cloud (2008, background): “The first core at its formation epoch has a mass of 5:1 ; 10 3 M and a radius of R ’ 0:71 AU, which is equivalent to or slightly larger than that expected by onedimensional radiation hydrodynamic calculations (Masunaga & Inutsuka 2000).”
Molecular Evolution and Star Formation: From Prestellar Cores to Protostellar Cores (2007, methodology): “Masunaga & Inutsuka (2000) calculated two models with different initial conditions: a homogeneous core (one of uniform density) and a hydrostatic core (a Bonnor-Ebert sphere).”
The physics of star formation (2003, background): “…the dust, which then controls the temperature by its strongly temperature-dependent thermal emission, maintaining a low and almost constant temperature of about 10 K over a wide range of densities (Hayashi and Nakano 1965; Hayashi 1966; Larson 1973, 1985; Tohline 1982; Masunaga and Inutsuka 2000).”
Simulating star formation in molecular cloud cores. I. The influence of low levels of turbulence on fragmentation and multiplicity (2003, background): “For cores with mass in the range 1 to 10M⊙ and initial temperatureT ∼ 10 K, the switch from isothermality to adiabaticity occurs at a critical densityρcrit ∼ 10−13 g cm−3 (Larson 1969; Tohline 1982; Masunaga & Inutsuka 2000).”
The formation of a star cluster: predicting the properties of stars and brown dwarfs (2002, methodology): “For standard molecular gas at an initial temperature of 10 K the gas begins to heat significantly at a density of ≈ 10−13 g cm−3 (Larson 1969; Masunaga & Inutsuka 2000).”
ANALYTICAL THEORY FOR THE INITIAL MASS FUNCTION. II. PROPERTIES OF THE FLOW (2009, positive): “Various authors (e.g. Glover & Mac Low 2007) found that for densities smaller than n̄ ≃ 105 cm−3, i.e. ρ̄ ∼ 10−18 g cm−3, the effective polytropic exponent is about γ ≃ 0.7, whereas at higher densities γ ≃ 1 (Masunaga & Inutsuka 2000).”
Molecular Evolution in Collapsing Prestellar Cores (2001, positive): “Numerical simulations show that the inner region of this solution is a good approximation for the “first collapse” phase of protostar formation (Masunaga et al. 1998; Masunaga & Inutsuka 2000).”
Magnetic processes in a collapsing dense core I. Accretion and ejection (2007, background): “In particular the second collapse is not considered here (Masunaga & Inutsuka 2000, Machida et al. 2007).”
Stellar, brown dwarf and multiple star properties from hydrodynamical simulations of star cluster formation (2008, methodology): “This equation of state has been chosen to match closely the relationship between temperature and density during the spherically-symmetric collapse of molecular cloud cores with solar metallicity as calculated with frequency-dependent radiative transfer (e.g., Masunaga & Inutsuka 2000).”
The thermodynamics of collapsing molecular cloud cores using smoothed particle hydrodynamics with radiative transfer (2005, methodology): “The latter is usually based on the evolution of the temperature at the highest density during the collapse of spherically symmetric clouds as calculated using radiative transfer (e.g. Larson 1969; Winkler & Newman 1980; Masunaga & Inutsuka 2000).”