Monte Carlo radiative transfer in SPH density fields

Abstract

We combine a Monte Carlo radiative transfer code with an SPH code, so that -- assuming thermal equilibrium -- we can calculate dust-temperature fields, spectral energy distributions, and isophotal maps, for the individual time-frames generated by an SPH simulation. On large scales, the radiative transfer cells (RT cells) are borrowed from the tree structure built by the SPH code, and are chosen so that their size -- and hence the resolution of the calculated temperature field -- is comparable with the resolution of the density field. We refer collectively to these cubic RT cells as the 'global grid'. The code is tested and found to treat externally illuminated dust configurations very well. However, when there are embedded discrete sources, i.e. stars, these produce very steep local temperature gradients which can only be modelled properly if -- in the immediate vicinity of, and centred on, each embedded star -- we supplement the global grid with a 'star grid' of closely spaced concentric RT cells.

arXiv commentAccepted by A&A

References in corpus (12)

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Cited by in corpus (21)

• Sunrise: Polychromatic Dust Radiative Transfer in Arbitrary Geometries
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• Astrophysical Smooth Particle Hydrodynamics
• Radiative transfer and the energy equation in SPH simulations of star formation
• TRAPHIC - Radiative Transfer for Smoothed Particle Hydrodynamics Simulations
• Introducing a Hybrid Method of Radiative Transfer for Smoothed Particle Hydrodynamics
• SPHRAY: A Smoothed Particle Hydrodynamics Ray Tracer for Radiative Transfer
• Using hierarchical octrees in Monte Carlo radiative transfer simulations
• The dust temperatures of the prestellar cores in the rho Oph main cloud and in other star forming regions: consequences for the core mass function
• Using 3D Voronoi grids in radiative transfer simulations
• Identifying and Analysing Protostellar Disc Fragments in Smoothed Particle Hydrodynamics Simulations
• Dynamic Monte Carlo radiation transfer in SPH. Radiation pressure force implementation
• How to identify the youngest protostars
• Panchromatic Spectral Energy Distributions of Dusty Galaxies with RADISHE. I. Predictions for Herschel: Correlating Colors with Galactic Energy Sources
• Observational signatures of outbursting protostars -- II: Exploring a wide range of eruptive protostars
• Observational signatures of outbursting protostars - I: From hydrodynamic simulations to observations
• MODA: a new algorithm to compute optical depths in multi-dimensional hydrodynamic simulations
• Modelling Herschel observations of infrared-dark clouds in the Hi-GAL survey
• SPAMCART: a code for smoothed particle Monte Carlo radiative transfer
• Native Synthetic Imaging of Smoothed Particle Hydrodynamics density fields using gridless Monte Carlo Radiative Transfer
• Observational characteristics of dense cores with deeply embedded young protostars