HERACLES: a three-dimensional radiation hydrodynamics code

González, M.; Audit, E.; Huynh, Philippe

doi:10.1051/0004-6361:20065486

Cited by 221 publications

(285 citation statements)

References 29 publications

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“…The spike's amplitude varies according to the model used for radiation and to the effective numerical resolution. Thanks to the AMR scheme, the spike's amplitude is larger in the supercritical case, but not as large as those obtained with M1 or VTEF models (Hayes & Norman 2003;González et al 2007). However, this last test shows the ability of our time-splitting method to integrate the RHD equations.…”

Section: D Full Rhd Tests: Radiative Shocksmentioning

confidence: 68%

Radiation hydrodynamics with adaptive mesh refinement and application to prestellar core collapse

Commerçon

Teyssier²,

Audit³

et al. 2011

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Context. Radiative transfer has a strong impact on the collapse and the fragmentation of prestellar dense cores. Aims. We present the radiation-hydrodynamics (RHD) solver we designed for the RAMSES code. The method is designed for astrophysical purposes, and in particular for protostellar collapse. Methods. We present the solver, using the co-moving frame to evaluate the radiative quantities. We use the popular flux-limited diffusion approximation under the grey approximation (one group of photons). The solver is based on the second-order Godunov scheme of RAMSES for its hyperbolic part and on an implicit scheme for the radiation diffusion and the coupling between radiation and matter. Results. We report in detail our methodology to integrate the RHD solver into RAMSES. We successfully test the method in several conventional tests. For validation in 3D, we perform calculations of the collapse of an isolated 1 M prestellar dense core without rotation. We successfully compare the results with previous studies that used different models for radiation and hydrodynamics. Conclusions. We have developed a full radiation-hydrodynamics solver in the RAMSES code that handles adaptive mesh refinement grids. The method is a combination of an explicit scheme and an implicit scheme accurate to the second-order in space. Our method is well suited for star-formation purposes. Results of multidimensional dense-core-collapse calculations with rotation are presented in a companion paper.

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Section: D Full Rhd Tests: Radiative Shocksmentioning

confidence: 68%

Radiation hydrodynamics with adaptive mesh refinement and application to prestellar core collapse

Commerçon

Teyssier²,

Audit³

et al. 2011

A&A

Self Cite

158

174

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“…We use a closure relation introduced by Dubroca & Feugeas (1999). The M1 method is used in the RHD code HERACLES (González et al 2007). Based on a minimum entropy principle, which is a method able to account for the large anisotropy of the radiation, as well as for the correct diffusion limit.…”

Section: M1 Modelmentioning

confidence: 99%

Physical and radiative properties of the first-core accretion shock

Commerçon

Audit

Chabrier

et al. 2011

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Context. Radiative shocks play a dominant role in star formation. The accretion shocks on first and second Larson cores involve radiative processes and are thus characteristic of radiative shocks. Aims. In this study, we explore the formation of the first Larson core and characterize the radiative and dynamical properties of the accretion shock, using both analytical and numerical approaches. Methods. We developed both numerical radiation-hydrodynamics calculations and a semi-analytical model that characterize radiative shocks in various physical conditions, for radiating or barotropic fluids. Then, we performed 1D spherical collapse calculations of the first Larson core, using a grey approximation for the opacity of the material. We considered three different models for radiative transfer: the barotropic approximation, the flux limited diffusion approximation, and the more complete M1 model. We investigate the characteristic properties of the collapse and of the first core formation. Comparison between the numerical results and our semianalytical model for radiative shocks shows that the latter reproduces the core properties obtained with the numerical calculations quite well. Results. The accretion shock on the first Larson core is found to be supercritical; i.e., the post and pre-shock temperatures are equal, implying that all the accretion shock energy on the core is radiated away. The shock properties are described well by the semianalytical model. The flux-limited diffusion approximation is found to agree quite well with the results based on the M1 model of radiative transfer, and is thus appropriate for studying the star formation process and allows a tractable and relatively correct treatment of radiative transfer in multidimensional radiation-hydrodynamics calculations. In contrast, the barotropic approximation does not correctly describe the thermal properties of the gas during the collapse.

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“…Over the past few years, several accretion disc simulations have been performed using similar numerical schemes (Turner 2004;Hirose et al 2006;Blaes et al 2007;Krolik et al 2007;Flaig et al 2009) and have recently included irradiation heating (Hirose & Turner 2011). More sophisticated radiation hydrodynamics (RHD) methods, like the two-moment method (González et al 2007), are usually very time demanding because they require large matrix inversion. In this work we develop a radiative transfer method based on the two-temperature grey 1 FLD approach by Commerçon et al (2011) and the hybdrid FLD approach (Kuiper et al 2010) that includes frequency dependent irradiation by the star.…”

Section: Introductionmentioning

confidence: 99%

Radiation magnetohydrodynamics in global simulations of protoplanetary discs

Flock

Fromang

González

et al. 2013

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Aims. Our aim is to study the thermal and dynamical evolution of protoplanetary discs in global simulations, including the physics of radiation transfer and magneto-hydrodynamic turbulence caused by the magneto-rotational instability. Methods. We have developed a radiative transfer method based on the flux-limited diffusion approximation that includes frequency dependent irradiation by the central star. This hybrid scheme is implemented in the PLUTO code. The focus of our implementation is on the performance of the radiative transfer method. Using an optimized Jacobi preconditioned BiCGSTAB solver, the radiative module is three times faster than the magneto-hydrodynamic step for the disc set-up we consider. We obtain weak scaling efficiencies of 70% up to 1024 cores. Results. We present the first global 3D radiation magneto-hydrodynamic simulations of a stratified protoplanetary disc. The disc model parameters were chosen to approximate those of the system AS 209 in the star-forming region Ophiuchus. Starting the simulation from a disc in radiative and hydrostatic equilibrium, the magneto-rotational instability quickly causes magneto-hydrodynamic turbulence and heating in the disc. We find that the turbulent properties are similar to that of recent locally isothermal global simulations of protoplanetary discs. For example, the rate of angular momentum transport α is a few times 10 −3 . For the disc parameters we use, turbulent dissipation heats the disc midplane and raises the temperature by about 15% compared to passive disc models. The vertical temperature profile shows no temperature peak at the midplane as in classical viscous disc models. A roughly flat vertical temperature profile establishes in the optically thick region of the disc close to the midplane. We reproduce the vertical temperature profile with viscous disc models for which the stress tensor vertical profile is flat in the bulk of the disc and vanishes in the disc corona. Conclusions. The present paper demonstrates for the first time that global radiation magneto-hydrodynamic simulations of turbulent protoplanetary discs are feasible with current computational facilities. This opens up the window to a wide range of studies of the dynamics of the inner parts of protoplanetary discs, for which there are significant observational constraints.

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HERACLES: a three-dimensional radiation hydrodynamics code

Cited by 221 publications

References 29 publications

Radiation hydrodynamics with adaptive mesh refinement and application to prestellar core collapse

Radiation hydrodynamics with adaptive mesh refinement and application to prestellar core collapse

Physical and radiative properties of the first-core accretion shock

Radiation magnetohydrodynamics in global simulations of protoplanetary discs

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