The dusty MOCASSIN: fully self-consistent 3D photoionization and dust radiative transfer models
By Barbara Ercolano, M. Barlow, P. Storey. 2005
147 citations recorded by the source corpus.
We present the first 3D Monte Carlo (MC) photoionization code to include a fully self-consistent treatment of dust radiative transfer (RT) within a photoionized region. This is the latest development (version 2.0) of the gas-only photoionization code MOCASSIN and employs a stochastic approach to the transport of radiation, allowing both the primary and secondary components of the radiation field to be treated self-consistently, whilst accounting for the scattering of radiation by dust grains mixed with the gas, as well as the absorption and emission of radiation by both the gas and the dust components. An escape probability method is implemented for the transfer of resonance lines that may be absorbed by the grains, thus contributing to their energy balance. The energetics of the co-existing dust and gas components must also take into account the effects of dust‐gas collisions and photoelectric emission from the dust grains, which are dependent on the grain charge. These are included in our code using the average grain potential approximation scheme. A set of rigorous benchmark tests have been carried out for dust-only spherically symmetric geometries and 2D disc configurations. The results of MOCASSIN are found to be in agreement with those obtained by well-established dust-only RT codes that employ various approaches to the solution of the RT problem. A model of the dust and of the photoionized gas components of the planetary nebula NGC 3918 is also presented as a means of testing the correct functioning of the RT procedures in a case where both gas and dust opacities are present. The two components are coupled via the heating of dust grains by the absorption of both UV continuum photons and resonance line photons emitted by the gas. The MOCASSIN results show agreement with those of a 1D dust and gas model of this nebula published previously, showing the reliability of the new code, which can be applied to a variety of astrophysical environments. Ke yw ords: radiative transfer ‐ dust, extinction ‐ H II regions ‐ planetary nebulae: general.
View Paper: https://www.semanticscholar.org/paper/8654d95eff3f1860b0f656304d2464ff5b51272c
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- J. Owen
- C. Clarke
- Barbara Ercolano
- James E. Owen
- Ian A. Bonnell
- J. Dale
- Jens Kauffmann
- Mark R. Krumholz
Citations in the corpus
- X-Ray-Irradiated Protoplanetary Disk Atmospheres. I. Predicted Emission-Line Spectrum and Photoevaporation (2008, methodology): “…and self-consistent model of irradiated gaseous T Tauri disks, we employ a fully 3D photoionisation and dust radiative transfer code, mocassin (Ercolano et al., 2003, 2005, 2008), to calculate the detailed ionisation and temperature structure of a typical T Tauri disk, with special emphasis…”
- Protoplanetary disc evolution and dispersal: the implications of X-ray photoevaporation (2010, methodology): “(Stone & Norman 1992) to calculate the hydrodynamical evolution of the disc, where the gas temperature due to Xray irradiation is parametrised as a function of ionisation parameter using the 3D radiative transfer code mocassin (Ercolano et al 2003, 2005, 2008).”
- Massive stars in massive clusters II: Disruption of bound clusters by photoionization (2012, methodology): “We will describe this technique in detail in Dale and Ercolano (2012), in prep, and validate it by comparison with the Monte Carlo radiative transfer code mocassin (Ercolano et al. 2003, 2005, 2008).”
- THE EFFECT OF LINE-OF-SIGHT TEMPERATURE VARIATION AND NOISE ON DUST CONTINUUM OBSERVATIONS (2009, methodology): “We thus use the radiative transfer code MOCASSIN (Ercolano et al. 2005).”
- Radiation-hydrodynamic models of X-ray and EUV photoevaporating protoplanetary discs (2009, methodology): “This parametrization is based on the results of 3D Monte Carlo radiative transfer calculations us- c© 2002 RAS, MNRAS 000, 1–16 ing mocassin (Ercolano et al. 2003, 2005, 2008a).”