The thermodynamics of collapsing molecular cloud cores using smoothed particle hydrodynamics with radiative transfer

By S. Whitehouse, Matthew R. Bate. 2005

140 citations recorded by the source corpus.

We present the results of a series of calculations studying the collapse of molecular cloud cores performed using a three-dimensional smoothed particle hydrodynamics code with radiative transfer in the flux-limited diffusion approximation. The opacities and specific heat capacities are identical for each calculation. However, we find that the temperature evolution during the simulations varies significantly when starting from different initial conditions. Even spherically symmetric clouds with different initial densities show markedly different development. We conclude that simple barotropic equations of state like those used in some previous calculations provide at best a crude approximation to the thermal behaviour of the gas. Radiative transfer is necessary to obtain accurate temperatures.

Subfields: Applied Mathematics, Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics

View Paper: https://www.semanticscholar.org/paper/b82cfd89c7182da5509f052871fa9b2f8425eb9f

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In Applied Mathematics

In Astronomy and Astrophysics

In Atomic and Molecular Physics, and Optics

Citations in the corpus

The effect of magnetic fields on star cluster formation (2008, background): “…incorporate a self-consistent treatment of radiative ransfer (in the flux-limited diffusion approximation) rather than ab rytropic equation of state (Whitehouse & Bate 2006) that a fulltreatment will affect fragmentation where the assumption of spherical symmetry is poor and in the region…”
Radiative transfer and the energy equation in SPH simulations of star formation (2007, methodology): “(ii) In the Whitehouse & Bate (2006) simulation the centre of the cloud heats up more rapidly at densities ρ ∼ 10−11 to 10−6 g cm−3, i.e. at lower densities than in our simulation.”
The properties of brown dwarfs and low-mass hydrogen-burning stars formed by disc fragmentation (2008, methodology): “However, these simulations have been performed with a barotropic equation of state, and therefore the effects of radiative transfer (e.g. Boss et al. 2000; Whitehouse & Bate 2006; Stamatellos et al. 2007a) are not properly captured.”
On the diversity and statistical properties of protostellar discs (2018, methodology): “…(SPH) code, sphNG, based on the original version of Benz (1990; Benz et al. 1990), but substantially modified using the methods described in Bate et al. (1995), Price & Monaghan (2007), Whitehouse, Bate & Monaghan (2005), Whitehouse & Bate (2006) and parallelised using both OpenMP and MPI.”
The First Stellar Cluster (2007, background): “In particular, the existence of a strict relationship between temperature and density is unlikely, even when the cooling time of the gas is short compared to the dynamical time (Whitehouse & Bate 2006).”
The importance of radiative feedback for the stellar initial mass function (2008, methodology): “Further details on the implementation of the equation of state can be found in Whitehouse & Bate (2006).”
Astrophysical smooth particle hydrodynamics (2009, methodology): “Flux-limited diffusion schemes have been suggested by Whitehouse et al. (2005), Whitehouse and Bate (2006) and Mayer et al. (2007), Monte-Carlo-type approaches have been followed by Oxley and Woolfson (2003), Stamatellos and Whitworth (2005), Semelin et al. (2007), and Croft and Altay (2008) and…”
Stellar, brown dwarf and multiple star properties from hydrodynamical simulations of star cluster formation (2008, background): “Whitehouse & Bate (2006) showed that replacing the barotropic equation of state by radiative transfer can lead to temperatures up to an order of magnitude higher near young low-mass protostars and, thus, potentially strongly inhibits fragmentation.”
Stellar, brown dwarf and multiple star properties from a radiation hydrodynamical simulation of star cluster formation (2011, methodology): “…smoothed particle hydrodynamics (SPH) code based on the original version of Benz (1990; Benz et al. 1990), but substantially modified as described in Bate et al. (1995), Whitehouse, Bate & Monaghan (2005), Whitehouse & Bate (2006), Price & Bate (2007), and parallelized using both OpenMP and MPI.”
Smoothed Particle Hydrodynamics in Astrophysics (2010, background): “Perhaps the simplest and also oldest approaches are based onflux-limited diffusion approximations to radiative transfer in SPH (Whitehouse & Bate, 2004; Whitehouse, Bate & Monaghan, 2005; Whitehouse & Bate, 2006; Fryer, Rockefeller & Warren, 2006; Viau, Bastien & Cha, 2006; Forgan et al., 2009).”
Phantom: A Smoothed Particle Hydrodynamics and Magnetohydrodynamics Code for Astrophysics (2017, methodology): “It can be fixed by implementing radiative feedback, for example by implementing radiation hydrodynamics in the flux-limited diffusion approximation (Whitehouse & Bate, 2004; Whitehouse et al., 2005; Whitehouse & Bate, 2006).”
High- and Low-Velocity Magnetized Outflows in the Star Formation Process in a Gravitationally Collapsing Cloud (2008, background): “…bymany authors, including the detailed radiative process under spherical symmetry (e.g., Larson 1969; Tohline 1982;Winkler & Newman 1980a, 1980b; Masunaga et al. 1998; Masunaga & Inutsuka 2000), and in recent three-dimensional calculations (e.g., Whitehouse & Bate 2006; Stamatellos et al. 2007).”
THE EFFECTS OF RADIATIVE TRANSFER ON LOW-MASS STAR FORMATION (2009, methodology): “By modeling star formation with gray flux-limited diffusion (GFLD), it has been shown that a barotropic or polytropic equation of state (EOS) can underestimate the true heating at high densities even for simple, non-turbulent collapse problems (Boss et al. 2000; Whitehouse & Bate 2006).”
RADIATION MAGNETOHYDRODYNAMIC SIMULATIONS OF PROTOSTELLAR COLLAPSE: PROTOSTELLAR CORE FORMATION (2012, background): “…and structure of the first core are in good agreement with the results of the 1D spherically symmetric RHD simulations using full non-gray radiation transfer (Masunaga et al. 1998; Masunaga & Inutsuka 2000) and the 3D SPH RHD simulations using the gray FLD approximation (Whitehouse & Bate 2006).”
Gas- and dust evolution in protoplanetary disks (2010, background): “It should be noted that several groups perform 3D hydrodynamic simulations of collapsing cloud cores which show more complicated evolution (e.g.,Banerjee & Pudritz 2006; Whitehouse & Bate 2006).”
Theory of Star Formation (2007, background): “Simulations are as yet inadequate to evaluate the effectiveness of this process in producing brown dwarfs; in particular, it is important to include proper treatment of the radiative transfer (Boss et al., 2000; Whitehouse & Bate, 2006).”
THE ISOTROPIC DIFFUSION SOURCE APPROXIMATION FOR SUPERNOVA NEUTRINO TRANSPORT (2007, background): “…2006) to cosmology (Bonanno & Romano 1994), including areas such as accretion discs, both around stars (Kley 1989) and more energetic objects where the accretion disc is dominated by radiation (e.g. (Turner et al. 2002; Hujeirat & Camenzind 2000)), and star formation (Whitehouse & Bate 2006).”