Smoothed particle hydrodynamics with radiative transfer in the flux-limited diffusion approximation

By S. Whitehouse, Matthew R. Bate. 2004

135 citations recorded by the source corpus.

We describe the implementation and testing of a smoothed particle hydrodynamics (SPH) code that solves the equations of radiation hydrodynamics in the flux-limited diffusion (FLD) approximation. The SPH equations of radiation hydrodynamics for an explicit integration scheme are derived and tested. We also discuss the implementation of an implicit numerical scheme for solving the radiation equations that allows the system to be evolved using time-steps much longer than the explicit radiation time-step. The code is tested on a variety of one-dimensional radiation hydrodynamics problems including radiation propagating in an optically thin medium, optically thick and thin shocks, subcritical and supercritical radiating shocks, and a radiation dominated shock. Many of the tests were also performed by Turner & Stone to test their implementation of a FLD module for the zeus-2d code. The SPH code performs at least as well as the zeus-2d code in these tests.

Subfields: Computational Mechanics, Ocean Engineering

View Paper: https://www.semanticscholar.org/paper/dfbb4e13685f4a4c38572424ba6261fe0b84e24c

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Citations in the corpus

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).”
Radiative transfer and the energy equation in SPH simulations of star formation (2007, background): “Radiative transfer (RT) has only recently been included in SPH codes (Oxley & Woolfson 2003; Whitehouse & Bate 2004, 2006; Whitehouse et al. 2005; Viau et al. 2005; Mayer et al. 2007).”
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).”
The importance of radiative feedback for the stellar initial mass function (2008, methodology): “Two temperature (gas and radiation) radiative transfer in the flux-limited diffusion approximation is implemented as described by Whitehouse et al. (2005) and Whitehouse & Bate (2006).”
Astrophysical smooth particle hydrodynamics (2009, unknown): “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…”
On the diversity and statistical properties of protostellar discs (2018, methodology): “The calculation employed two temperature (gas and radiation) radiative transfer in the flux-limited diffusion approximation (Whitehouse et al. 2005; Whitehouse & Bate 2006).”
Smoothed particle hydrodynamics and magnetohydrodynamics (2010, background): “, 2002; Hu and Adams, 2006), salt diffusion (Monaghan, Huppert, and Worster, 2005) and in an astrophysical context for the treatment of radiation in the Flux-Limited Diffusion approximation (Whitehouse and Bate, 2004; Whitehouse et al., 2005).”
Equations and Algorithms for Mixed-frame Flux-limited Diffusion Radiation Hydrodynamics (2006, background): “Comparison to Comoving Frame Formulations Many popular numerical treatments of radiation hydrodynamics (e.g. Turner & Stone 2001; Whitehouse & Bate 2004; Hayes et al. 2006) use a comoving formulation of the equations rather than our mixed frame formulation.”
The thermodynamics of collapsing molecular cloud cores using smoothed particle hydrodynamics with radiative transfer (2005, background): “Despite these advantages, few attempts have been made to include radiative transfer into SPH (Lucy 1977; Brookshaw 1985, 1986; Oxley & Woolfson 2003; Whitehouse & Bate 2004), and until recently (Bastien, Cha & Viau 2004, 2005) SPH with radiative transfer has not been applied to star formation.”
The effect of magnetic fields on star cluster formation (2008, background): “…Monaghan (2002) and Price & Monaghan (2004b) and by the introduction of additional physics in the form of magnetic fields (Price & Bate 2007) and radiative transfer using the flux-limited diffusion approximation (Whitehouse et al. 2005) (although we do not include radiative transfer in this paper).”
Stellar, brown dwarf and multiple star properties from a radiation hydrodynamical simulation of star cluster formation (2011, methodology): “Two temperature (gas and radiation) radiative transfer in the fluxlimited diffusion approximation is implemented as described by Whitehouse et al. (2005) and Whitehouse & Bate (2006), except that the standard explicit SPH contributions to the gas energy equation due to the work and artificial…”