Protostellar collapse: radiative and magnetic feedbacks on small scale fragmentation

Abstract

It is established that both radiative transfer and magnetic field have a strong impact on the collapse and the fragmentation of prestellar dense cores, but no consistent calculation exists yet at such scales. We present original AMR calculations including magnetic field (in the ideal MHD limit) and radiative transfer, within the Flux Limited Diffusion approximation, of the collapse of a 1 solar mass dense core. We compare the results with calculations performed with a barotropic EOS. We show that radiative transfer has an important impact on the collapse and the fragmentation, through the cooling or heating of the gas, and is complementary of the magnetic field. A larger field yields a stronger magnetic braking, increasing the accretion rate and thus the effect of the radiative feedback. Even for a strongly magnetized core, where the dynamics of the collapse is dominated by the magnetic field, radiative transfer is crucial to determine the temperature and optical depth distributions, two potentially accessible observational diagnostics. A barotropic EOS cannot account for realistic fragmentation. The diffusivity of the numerical scheme, however, is found to strongly affect the output of the collapse, leading eventually to spurious fragmentation. Both radiative transfer and magnetic field must be included in numerical calculations of star formation to obtain realistic collapse configurations and observable signatures. Nevertheless, the numerical resolution and the robustness of the solver are of prime importance to obtain reliable results. When using an accurate solver, the fragmentation is found to always remain inhibited by the magnetic field, at least in the ideal MHD limit, even when radiative transfer is included.

6 pages, 7 figures, accepted for publication in Astronomy and Astrophysics

References in corpus (12)

• A High Order Godunov Scheme with Constrained Transport and Adaptive Mesh Refinement for Astrophysical MHD
• Radiation-Hydrodynamic Simulations of Collapse and Fragmentation in Massive Protostellar Cores
• The Effects of Radiative Transfer on Low-Mass Star Formation
• Magnetic processes in a collapsing dense core. I Accretion and Ejection
• The Importance of Radiative Feedback for the Stellar Initial Mass Function
• The impact of magnetic fields on single and binary star formation
• Magnetic processes in a collapsing dense core. II Fragmentation. Is there a fragmentation crisis ?
• The effect of magnetic fields on star cluster formation
• Protostellar collapse: radiative and magnetic feedbacks on small scale fragmentation
• Formation Scenario for Wide and Close Binary Systems
• Protostellar collapse: A comparison between SPH and AMR calculations
• Simulating star formation in molecular cloud cores IV. The role of turbulence and thermodynamics

Cited by in corpus (110)

• Stellar Multiplicity
• Stellar, brown dwarf and multiple star properties from a radiation hydrodynamical simulation of star cluster formation
• Protostellar disk formation and transport of angular momentum during magnetized core collapse
• Radiation Magnetohydrodynamic Simulations of Protostellar Collapse: Protostellar Core Formation
• Collapse of massive magnetized dense cores using radiation-magneto-hydrodynamics: early fragmentation inhibition
• The Interplay of Magnetic Fields, Fragmentation and Ionization Feedback in High-Mass Star Formation
• Ambipolar diffusion in low-mass star formation. I. General comparison with the ideal MHD case
• Collapse, outflows and fragmentation of massive, turbulent and magnetized prestellar barotropic cores
• Radiation Magnetohydrodynamic Simulations of Protostellar Collapse: Non-Ideal Magnetohydrodynamic Effects and Early Formation of Circumstellar Disks
• Modeling jet and outflow feedback during star cluster formation
• The earliest phases of star formation - A Herschel key project. The thermal structure of low-mass molecular cloud cores
• Can non-ideal magnetohydrodynamics solve the magnetic braking catastrophe?
• Observed luminosity spread in young clusters and Fu Ori stars: a unified picture
• Protostellar collapse: radiative and magnetic feedbacks on small scale fragmentation
• Radiation hydrodynamics with Adaptive Mesh Refinement and application to prestellar core collapse. I Methods
• Local outflows from turbulent accretion disks
• Collapse of a molecular cloud core to stellar densities: stellar core and outflow formation in radiation magnetohydrodynamics simulations
• Conditions for Circumstellar Disk Formation: Effects of Initial Conditions and Sink Treatment
• Evolution of Protostellar Outflow around Low-mass Protostar
• The influence of turbulence during magnetized core collapse and its consequences on low-mass star formation
• Radiation-Hydrodynamic Simulations of the Formation of Orion-Like Star Clusters I. Implications for the Origin of the Initial Mass Function
• Turbulence-induced disc formation in strongly magnetised cloud cores
• The Origin and Formation of the Circumstellar Disk
• Disc formation in turbulent massive cores: Circumventing the magnetic braking catastrophe
• Analytical theory for the initial mass function: III time dependence and star formation rate
• On the Stability of Non Force-Free Magnetic Equilibria in Stars
• The enigmatic core L1451-mm: a first hydrostatic core? or a hidden VeLLO?
• Protostellar birth with ambipolar and ohmic diffusion
• Magnetic fields during the early stages of massive star formation - II. A generalised outflow criterion
• Radiation Magnetohydrodynamics Simulation of Proto-Stellar Collapse: Two-Component Molecular Outflow
• Forming spectroscopic massive proto-binaries by disk fragmentation
• Collapse of a molecular cloud core to stellar densities: the formation and evolution of pre-stellar discs
• The Formation of Population III Stars in Gas Accretion Stage: Effects of Magnetic Fields
• A chemical solver to compute molecule and grain abundances and non-ideal MHD resistivities in prestellar core collapse calculations
• The role of magnetic fields in the formation of protostellar discs
• Importance of the Initial Conditions for Star Formation - II. Fragmentation Induced Starvation and Accretion Shielding
• The importance of magnetic fields for the initial mass function of the first stars
• Simulations of protostellar collapse using multigroup radiation hydrodynamics. II. The second collapse
• There is no magnetic braking catastrophe: Low-mass star cluster and protostellar disc formation with non-ideal magnetohydrodynamics
• Exposed Long-lifetime First-core: A New Model of First Cores Based on Radiation Hydrodynamics
• Physical Processes in Star Formation
• Collimated jets from the first core
• On the stability of radiation-pressure-dominated cavities
• The impact of the Hall effect during cloud core collapse:implications for circumstellar disk evolution
• Synthetic observations of first hydrostatic cores in collapsing low-mass dense cores. I. Spectral energy distributions and evolutionary sequence
• Accretion and magnetic field morphology around Class 0 stage protostellar discs
• The nonisothermal stage of magnetic star formation. II. Results
• The collapse of a molecular cloud core to stellar densities using radiation non-ideal magnetohydrodynamics
• Impact of Protostellar Outflow on Star Formation: Effects of Initial Cloud Mass
• A fast, robust, and simple implicit method for adaptive time-stepping on adaptive mesh-refinement grids
• Zooming in on Individual Star Formation: Low- and High-mass Stars
• Revealing the dynamics of Class 0 protostellar discs with ALMA
• Stellar mass spectrum within massive collapsing clumps I. Influence of the initial conditions
• The lower limits of disc fragmentation and the prospects for observing fragmenting discs
• Physical and radiative properties of the first core accretion shock
• Protostellar collapse: the conditions to form dust rich protoplanetary disks
• Survival of interstellar molecules to prestellar dense core collapse and early phases of disk formation
• Simulations of protostellar collapse using multigroup radiation hydrodynamics. I. The first collapse
• Chemical and physical characterization of collapsing low-mass prestellar dense cores
• A Semi-Analytical Description for the Formation and Gravitational Evolution of Protoplanetary Disks
• The effect of episodic accretion on the phase transition of CO and CO_2 in low-mass star formation
• A grid of 1D low-mass star formation collapse models
• Impact of the Hall effect in star formation and the issue of angular momentum conservation
• Chemistry in the First Hydrostatic Core Stage By Adopting Three-Dimensional Radiation Hydrodynamic Simulations
• ALMA High Angular Resolution Polarization Study; An Extremely Young Class 0 Source, OMC-3/MMS 6
• Protostellar collapse and fragmentation using an MHD GADGET
• Multigroup radiation hydrodynamics with flux-limited diffusion and adaptive mesh refinement
• Hall effect-driven formation of gravitationally unstable discs in magnetized molecular cloud cores
• The effect of extreme ionisation rates during the initial collapse of a molecular cloud core
• The dynamical state of the First Hydrostatic Core Candidate Cha-MMS1
• Fossil field decay due to nonlinear tides in massive binaries
• On the fragmentation boundary in magnetised self-gravitating discs
• The magnetic diffusivities in 3D radiative chemo-hydrodynamic simulations of protostellar collapse
• Origin of Molecular Outflow Determined from Thermal Dust Polarization
• Protostellar collapse of magneto-turbulent cloud cores: shape during collapse and outflow formation
• Does turbulence determine the initial mass function?
• Dimensional argument for the impact of turbulent support on the stellar initial mass function
• Accuracy and Efficiency of Raytracing Photoionisation Algorithms
• Synthetic observations of first hydrostatic cores in collapsing low-mass dense cores II. Simulated ALMA dust emission maps
• The Properties of Prestellar Discs in Isolated and Multiple Prestellar Systems
• Spatially Resolving Substructures within the Massive Envelope around an Intermediate-mass Protostar: MMS 6/OMC-3
• The role of magnetic fields in the formation of multiple massive stars
• Mixing is easy: New insights for cosmochemical evolution from pre-stellar core collapse
• Evolution of Hubble wedges in episodic protostellar outflows
• From large-scale to protostellar disk fragmentation into close binary stars
• Role of environment and gas temperature in the formation of multiple protostellar systems: molecular tracers
• The dynamically young outflow of the Class 0 protostar Cha-MMS1
• Collapse and Fragmentation of Magnetic Molecular Cloud Cores with the Enzo AMR MHD Code. II. Prolate and Oblate Cores
• Fossil magnetic fields in intermediate-mass and massive stars
• Observational Identification of First Cores: Non-LTE Radiative Transfer Simulation
• Radiation Magnetohydrodynamic Simulations of Protostellar Collapse: Low-Metallicity Environments
• Investigating prescriptions for artificial resistivity in smoothed particle magnetohydrodynamics
• The Luminosity of Population III Star Clusters
• Radiation Hydrodynamics Simulations of Spherical Protostellar Collapse for Very Low Mass Objects
• Gravitational Collapse and Disk Formation in Magnetized Cores
• Protostellar disk accretion in turbulent filaments
• The formation of low-mass stars and brown dwarfs
• Insights into the first and second hydrostatic core stages from numerical simulations
• Formation of low-mass stars and brown dwarfs
• The factors that influence protostellar multiplicity I: Gas temperature, density, and mass in Perseus with Nobeyama
• Secular dipole-dipole stability of magnetic binaries
• A fast and accurate method of radiation hydrodynamics calculation in spherical symmetry
• Recent Developments in Simulations of Low-mass Star Formation
• Simulations of the IMF in Clusters
• Numerical Methods for Simulating Star Formation
• Radiative, magnetic and numerical feedbacks on small-scale fragmentation
• The 3D structure of disc-instability protoplanets
• Fast spectral line calculations with the escape probability method and tests with synthetic observations of interstellar clouds
• Discs and outflows in the early phases of massive star formation: influence of magnetic fields and ambipolar diffusion
• Dust coagulation during the early stages of star formation: molecular cloud collapse and first hydrostatic core evolution