The thermodynamics of collapsing molecular cloud cores using smoothed particle hydrodynamics with radiative transfer

Abstract

We present the results of a series of calculations studying the collapse of molecular cloud cores performed using a three-dimensional smoothed particle hydr odynamics code with radiative transfer in the flux-limited diffusion approximation. The opacities and specific heat capacities are identical for each calculation. However, we find that the temperature evolution during the simulations varies significantly when starting from different initial conditions. Even spherically-symmetric clouds with different initial densities show markedly different development. We conclude that simple barotropic equations of state like those used in some previous calculations provide at best a crude approximation to the thermal behaviour of the gas. Radiative transfer is necessary to obtain accurate temperatures.

8 pages, 9 figures, accepted for publication in MNRAS

References in corpus (2)

• A faster algorithm for smoothed particle hydrodynamics with radiative transfer in the flux-limited diffusion approximation
• Smoothed particle hydrodynamics with radiative transfer in the flux-limited diffusion approximation

Cited by in corpus (123)

• Theory of Star Formation
• Gas- and dust evolution in protoplanetary disks
• Stellar, brown dwarf and multiple star properties from a radiation hydrodynamical simulation of star cluster formation
• Stellar, Brown Dwarf, and Multiple Star Properties from Hydrodynamical Simulations of Star Cluster Formation
• Phantom: A smoothed particle hydrodynamics and magnetohydrodynamics code for astrophysics
• Radiation-Hydrodynamic Simulations of Collapse and Fragmentation in Massive Protostellar Cores
• Smoothed Particle Hydrodynamics in Astrophysics
• The properties of brown dwarfs and low-mass hydrogen-burning stars formed by disc fragmentation
• Formation of the First Stars
• On the diversity and statistical properties of protostellar discs
• The Big Problems in Star Formation: the Star Formation Rate, Stellar Clustering, and the Initial Mass Function
• The Effects of Radiative Transfer on Low-Mass Star Formation
• The Importance of Radiative Feedback for the Stellar Initial Mass Function
• Radiation Magnetohydrodynamic Simulations of Protostellar Collapse: Protostellar Core Formation
• The isotropic diffusion source approximation for supernova neutrino transport
• Astrophysical Smooth Particle Hydrodynamics
• Fragmentation of gravitationally unstable gaseous protoplanetary disks with radiative transfer
• The effect of magnetic fields on star cluster formation
• Circumplanetary disc properties obtained from radiation hydrodynamical simulations of gas accretion by protoplanets
• Formation Process of the Circumstellar Disk: Long-term Simulations in the Main Accretion Phase of Star Formation
• Radiative transfer and the energy equation in SPH simulations of star formation
• Protostellar collapse: radiative and magnetic feedbacks on small scale fragmentation
• Recurrent Planet Formation and Intermittent Protostellar Outflows Induced by Episodic Mass Accretion
• Radiation hydrodynamics with Adaptive Mesh Refinement and application to prestellar core collapse. I Methods
• Can giant planets form by gravitational fragmentation of discs?
• Collapse of a molecular cloud core to stellar densities: stellar core and outflow formation in radiation magnetohydrodynamics simulations
• Effects of Ohmic and ambipolar diffusion on the formation and evolution of the first cores, protostars and circumstellar discs
• Evolution of Protostellar Outflow around Low-mass Protostar
• Formation Scenario for Wide and Close Binary Systems
• Gas accretion onto planetary cores: three-dimensional self-gravitating radiation hydrodynamical calculations
• Inefficient star formation: The combined effects of magnetic fields and radiative feedback
• The Origin and Formation of the Circumstellar Disk
• The Internal Energy for Molecular Hydrogen in Gravitationally Unstable Protoplanetary Disks
• Radiation Feedback and Fragmentation in Massive Protostellar Cores
• TRAPHIC - Radiative Transfer for Smoothed Particle Hydrodynamics Simulations
• Driven and Decaying Turbulence Simulations of Low-Mass Star Formation: From Clumps to Cores to Protostars
• The statistical properties of stars and their dependence on metallicity
• Second Core Formation and High Speed Jets: Resistive MHD Nested Grid Simulations
• The statistical properties of stars and their dependence on metallicity: the effects of opacity
• The importance of episodic accretion for low-mass star formation
• Protostellar birth with ambipolar and ohmic diffusion
• Radiation Magnetohydrodynamics Simulation of Proto-Stellar Collapse: Two-Component Molecular Outflow
• Collapse of a molecular cloud core to stellar densities: the formation and evolution of pre-stellar discs
• A Quintet of Black Hole Mass Determinations
• Tidally induced brown dwarf and planet formation in circumstellar discs
• On the origin of the spiral morphology in the Elias 2-27 circumstellar disc
• Introducing a Hybrid Method of Radiative Transfer for Smoothed Particle Hydrodynamics
• The role of thermodynamics in disc fragmentation
• Exploring the conditions required to form giant planets via gravitational instability in massive protoplanetary discs
• On the Origin of Stellar Masses
• Testing Disk Instability Models for Giant Planet Formation
• 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
• Episodic accretion, protostellar radiative feedback, and their role in low-mass star formation
• Conditions for the Formation of First-Star Binaries
• The growth and hydrodynamic collapse of a protoplanet envelope
• Spitzer Observations of Bok Globule B335: Isolated Star Formation Efficiency and Cloud Structure
• The nonisothermal stage of magnetic star formation. II. Results
• The collapse of a molecular cloud core to stellar densities using radiation non-ideal magnetohydrodynamics
• Collapse of a molecular cloud core to stellar densities: the radiative impact of stellar core formation on the circumstellar disc
• Zooming in on Individual Star Formation: Low- and High-mass Stars
• The lower limits of disc fragmentation and the prospects for observing fragmenting discs
• Modeling UV Radiation Feedback from Massive Stars: I. Implementation of Adaptive Ray Tracing Method and Tests
• The Nonisothermal Stage of Magnetic Star Formation. I. Formulation of the Problem and Method of Solution
• Planet migration: self-gravitating radiation hydrodynamical models of protoplanets with surfaces
• Simulations of protostellar collapse using multigroup radiation hydrodynamics. I. The first collapse
• A Semi-Analytical Description for the Formation and Gravitational Evolution of Protoplanetary Disks
• The influence of the turbulent perturbation scale on prestellar core fragmentation and disk formation
• Disc formation and fragmentation using radiative non-ideal magnetohydrodynamics
• First Core Properties: From Low- to High-mass Star Formation
• Images of the radiatively inefficient accretion flow surrounding a Kerr black hole: application in Sgr A*
• Are Elias 2-27's spiral arms driven by self-gravity, or by a companion? A comparative spiral morphology study
• Dynamic Monte Carlo radiation transfer in SPH. Radiation pressure force implementation
• Combining radiative transfer and diffuse interstellar medium physics to model star formation
• Chemistry in the First Hydrostatic Core Stage By Adopting Three-Dimensional Radiation Hydrodynamic Simulations
• Flux-Limited Diffusion Approximation Models of Giant Planet Formation by Disk Instability
• Triggered fragmentation in self-gravitating discs: forming fragments at small radii
• Non-ideal magnetohydrodynamics vs turbulence I: Which is the dominant process in protostellar disc formation?
• The impact of non-ideal magnetohydrodynamic processes on discs, outflows, counter-rotation and magnetic walls during the early stages of star formation
• Hall effect-driven formation of gravitationally unstable discs in magnetized molecular cloud cores
• On the origin of magnetic fields in stars
• Birth of convective low-mass to high-mass second Larson cores
• A general hybrid radiation transport scheme for star formation simulations on an adaptive grid
• The young protostellar disk in IRAS16293-2422 B is hot and shows signatures of gravitational instability
• The dependence of protostar formation on the geometry and strength of the initial magnetic field
• Non-ideal magnetohydrodynamics vs turbulence II: Which is the dominant process in stellar core formation?
• Do we need non-ideal magnetohydrodynamics to model protostellar discs?
• Analytical Solutions for Radiative Transfer: Implications for Giant Planet Formation by Disk Instability
• The Properties of Prestellar Discs in Isolated and Multiple Prestellar Systems
• Shaken and stirred: the effects of turbulence and rotation on disc and outflow formation during the collapse of magnetised molecular cloud cores
• Arepo-MCRT: Monte Carlo Radiation Hydrodynamics on a Moving Mesh
• On the origin of magnetic fields in stars II: The effect of numerical resolution
• On the role of the H2 ortho:para ratio in gravitational collapse during star formation
• The statistical properties of stars at redshift, z=5, compared with the present epoch
• Mixing is easy: New insights for cosmochemical evolution from pre-stellar core collapse
• Efficient radiative transfer techniques in hydrodynamic simulations
• Sink particle radiative feedback in smoothed particle hydrodynamics models of star formation
• Chemo-dynamical simulations of dwarf galaxy evolution
• Synthetic molecular line observations of the first hydrostatic core from chemical calculations
• The statistical properties of protostellar discs and their dependence on metallicity
• Testing the accuracy of radiative cooling approximations in SPH simulations
• On the frequencies of circumbinary discs in protostellar systems
• Variation of the low-mass end of the stellar initial mass function with redshift and metallicity
• Migration of protoplanets with surfaces through discs with steep temperature gradients
• Formation of multiple low mass stars, brown dwarfs and planemos via gravitational collapse
• Formation of low mass protostars and their circumstellar disks
• Role of environment and gas temperature in the formation of multiple protostellar systems: molecular tracers
• The dependence of stellar properties on initial cloud density
• What can the SEDs of first hydrostatic core candidates reveal about their nature?
• Common envelopes in massive stars III. The obstructive role of radiation transport in envelope ejection
• Collapse and Fragmentation of Magnetic Molecular Cloud Cores with the Enzo AMR MHD Code. II. Prolate and Oblate Cores
• Native Synthetic Imaging of Smoothed Particle Hydrodynamics density fields using gridless Monte Carlo Radiative Transfer
• Turbulence and its connection to episodic accretion in binary YSOs
• Insights into the first and second hydrostatic core stages from numerical simulations
• How Does a Protostar Form by Magnetized Gravitational Collapse?
• Relativistic encounters in dense stellar systems
• Formation of accretion centers in simulations of colliding uniform density H${}_2$ cores
• The factors that influence protostellar multiplicity I: Gas temperature, density, and mass in Perseus with Nobeyama
• Holes within galaxies: the egg or the hen?
• Modelling dust coagulation, dynamical drag and turbulent mixing during star and disc formation
• Radiative, magnetic and numerical feedbacks on small-scale fragmentation
• The effects of a compressive velocity pulse on a collapsing turbulent clump