A new hybrid radiative transfer method for massive star formation

Abstract

Frequency-dependent/hybrid approaches for stellar irradiation are of primary importance in numerical simulations of massive star formation. We seek to compare outflow and accretion mechanisms in star formation simulations. We investigate the accuracy of a hybrid radiative transfer method using the gray M1 closure relation for proto-stellar irradiation and gray flux-limited diffusion (FLD) for photons emitted everywhere else. We have coupled the FLD module of the adaptive-mesh refinement code Ramses with Ramses-RT, which is based on the M1 closure relation. Our hybrid (M1+FLD) method takes an average opacity at the stellar temperature for the M1 module, instead of the local environmental radiation field. We have tested this approach in radiative transfer tests of disks irradiated by a star for three levels of optical thickness and compared the temperature structure with RADMC-3D and MCFOST. We applied it to a radiation-hydrodynamical simulation of massive star formation. Our tests validate our hybrid approach for determining the temperature structure of an irradiated disk in the optically-thin and moderately optically-thick regimes and the most optically-thick test shows the limitation of our approach. The optically-thick setups highlight the ability of the hybrid method to partially capture the self-shielding in the disk while the FLD cannot. The radiative acceleration is 100 times greater with the hybrid method. It consistently leads to about +50% more extended and wider-angle radiative outflows in the massive star formation simulation. We obtain a $17.6M_{\odot }$ at $t\simeq 0.7{\tau }_{\mathrm{ff}}$, while the accretion phase is ongoing. Finally, despite the use of refinement to resolve the radiative cavities, no Rayleigh-Taylor instability appears in our simulations, and we justify their absence by physical arguments based on the entropy gradient. (abridged)

arXiv comment17 pages, 17 figures, accepted for publication in A&A

References in corpus (50)

• Dust Grain Size Distributions and Extinction in the Milky Way, LMC, and SMC
• Cosmological Hydrodynamics with Adaptive Mesh Refinement: a new high resolution code called RAMSES
• Toward Understanding Massive Star Formation
• The Formation of Massive Stars from Turbulent Cores
• The Formation of Massive Star Systems by Accretion
• Rosseland and Planck Mean Opacities for Protoplanetary Discs
• High-Mass Star and Massive Cluster Formation in the Milky Way
• On the formation of massive stars
• A High Order Godunov Scheme with Constrained Transport and Adaptive Mesh Refinement for Astrophysical MHD
• Scattering by Interstellar Dust Grains. II. X-Rays
• Monte Carlo radiative transfer in protoplanetary disks
• Massive star formation: Nurture, not nature
• RAMSES-RT: Radiation hydrodynamics in the cosmological context
• Benchmark problems for continuum radiative transfer. High optical depths, anisotropic scattering, and polarisation
• The earliest phases of high-mass star formation: a 3 square degree millimeter continuum mapping of Cygnus X
• Protostellar disk formation and transport of angular momentum during magnetized core collapse
• Circumventing the radiation pressure barrier in the formation of massive stars via disk accretion
• Multi--dimensional Cosmological Radiative Transfer with a Variable Eddington Tensor Formalism
• The Shape of the Inner Rim in Proto-Planetary Disks
• Collapse of massive magnetized dense cores using radiation-magneto-hydrodynamics: early fragmentation inhibition
• Neutrino-driven convection versus advection in core collapse supernovae
• Equations and Algorithms for Mixed Frame Flux-Limited Diffusion Radiation Hydrodynamics
• Radiation hydrodynamics with Adaptive Mesh Refinement and application to prestellar core collapse. I Methods
• A radiative transfer scheme for cosmological reionization based on a local Eddington tensor
• Towards a more realistic sink particle algorithm for the RAMSES code
• The 2D Continuum Radiative Transfer Problem: Benchmark Results for Disk Configurations
• An Unstable Truth: How Massive Stars get their Mass
• Magnetically self-regulated formation of early protoplanetary discs
• First hydrodynamics simulations of radiation forces and photoionization feedback in massive star formation
• Galaxies that Shine: radiation-hydrodynamical simulations of disk galaxies
• AREPO-RT: Radiation hydrodynamics on a moving mesh
• Fast and accurate frequency-dependent radiation transport for hydrodynamics simulations in massive star formation
• Protostellar birth with ambipolar and ohmic diffusion
• Radiation Magnetohydrodynamics Simulation of Proto-Stellar Collapse: Two-Component Molecular Outflow
• Simulating the Formation of Massive Protostars: I. Radiative Feedback and Accretion Disks
• Simulations of protostellar collapse using multigroup radiation hydrodynamics. II. The second collapse
• Radiation hydrodynamics of triggered star formation: the effect of the diffuse radiation field
• On the simultaneous evolution of massive protostars and their host cores
• On the stability of radiation-pressure-dominated cavities
• Synthetic observations of first hydrostatic cores in collapsing low-mass dense cores. I. Spectral energy distributions and evolutionary sequence
• Modeling UV Radiation Feedback from Massive Stars: I. Implementation of Adaptive Ray Tracing Method and Tests
• Radiative Rayleigh-Taylor instabilities
• Radiation-hydrodynamical simulations of massive star formation using Monte Carlo radiative transfer II. The formation of a 25 solar-mass star
• Massive Star Formation via the Collapse of Subvirial and Virialized Turbulent Massive Cores
• Numerical Problems in Coupling Photon Momentum (Radiation Pressure) to Gas
• Hybrid Adaptive Ray-Moment Method (HARM${}^2$): A Highly Parallel Method for Radiation Hydrodynamics on Adaptive Grids
• Multigroup radiation hydrodynamics with flux-limited diffusion and adaptive mesh refinement
• Radiation hydrodynamics including irradiation and adaptive mesh refinement with AZEuS. I. Methods
• Radiative magneto-hydrodynamics in massive star formation and accretion disks
• The role of accretion disks in the formation of massive stars

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• A Massive Star is Born: How Feedback from Stellar Winds, Radiation Pressure, and Collimated Outflows Limits Accretion onto Massive Stars
• Collapse of turbulent massive cores with ambipolar diffusion and hybrid radiative transfer II. Outflows
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• Radiation-Hydrodynamics with MPI-AMRVAC: Flux-Limited Diffusion
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• How magnetic field and stellar radiative feedback influences the collapse and the stellar mass spectrum of a massive star forming clump
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• VETTAM: A scheme for radiation hydrodynamics with adaptive mesh refinement using the variable Eddington tensor method
• The role of magnetic fields in the formation of multiple massive stars
• Accuracy of ALMA estimates of young disk radii and masses. Predicted observations from numerical simulations
• Anatomy of the Class I protostar L1489 IRS with NOEMA -- I. Disk, streamers, outflow(s) and bubbles at 3mm
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• Disk fragmentation around a massive protostar: a comparison of two three-dimensional codes
• Physical conditions for dust grain alignment in Class 0 protostellar cores II. The role of the radiation field in models aligning/disrupting dust grains
• Discs are born eccentric
• The Role of Thermal Instability in Accretion Outbursts in High-Mass Stars
• Multidimensional half-moment multigroup radiative transfer. Improving moment-based thermal models of circumstellar disks
• New boundary conditions for the approximate flux-limited diffusion radiative transfer in circumstellar environments: test case study for spherically symmetric envelopes
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