Primordial magnetic fields in Population III star formation: a magnetised resolution study

Abstract

Population III stars form in groups due to the fragmentation of primordial gas. While uniform magnetic fields have been shown to support against fragmentation in present day star formation, it is unclear whether realistic k^3/2 primordial fields can have the same effect. We bypass the issues associated with simulating the turbulent dynamo by introducing a saturated magnetic field at equipartition with the velocity field when the central densities reaches 10-13 g cm-3. We test a range of sink particle creation densities from 10-10-10-8 g cm-3. Within the range tested, the fields did not suppress fragmentation of the gas and hence could not prevent the degree of fragmentation from increasing with increased resolution. The number of sink particles formed and total mass in sink particles was unaffected by the magnetic field across all seed fields and resolutions. The magnetic pressure remained sub-dominant to the gas pressure except in the highest density regions of the simulation box, where it became equal to but never exceeded gas pressure. Our results suggest that the inclusion of magnetic fields in numerical simulations of Pop III star formation is largely unimportant.

arXiv commentSubmitted to MNRAS

References in corpus (48)

• E pur si muove: Galiliean-invariant cosmological hydrodynamical simulations on a moving mesh
• Forming the First Stars in the Universe: The Fragmentation of Primordial Gas
• Thermal and Fragmentation Properties of Star-forming Clouds in Low-metallicity Environments
• Simulations on a Moving Mesh: The Clustered Formation of Population III Protostars
• The Protogalactic Origin for Cosmic Magnetic Fields
• The Formation and Fragmentation of Disks around Primordial Protostars
• Cosmological Formation of Low-Mass Objects
• Simulations of nonhelical hydromagnetic turbulence
• The Mass Spectrum of the First Stars
• Magnetic processes in a collapsing dense core. I Accretion and Ejection
• Magnetohydrodynamics on an unstructured moving grid
• Building up the Population III initial mass function from cosmological initial conditions
• Mach Number Dependence of Turbulent Magnetic Field Amplification: Solenoidal versus Compressive Flows
• Radiation Magnetohydrodynamic Simulations of Protostellar Collapse: Protostellar Core 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
• Hall magnetohydrodynamics of partially ionized plasmas
• The generation of strong magnetic fields during the formation of the first stars
• Small-scale dynamo action during the formation of the first stars and galaxies. I. The ideal MHD limit
• Magnetic processes in a collapsing dense core. II Fragmentation. Is there a fragmentation crisis ?
• Constraining the Statistics of Population III Binaries
• Magnetic Fields in Population III Star Formation
• Cosmological Magnetic Field: a fossil of density perturbations in the early universe
• Collapse and Fragmentation of Rotating Magnetized Clouds. II. Binary Formation and Fragmentation of First Cores
• The Small-Scale Dynamo and Non-Ideal MHD in Primordial Star Formation
• The Effects of Accretion Luminosity upon Fragmentation in the Early Universe
• Second Core Formation and High Speed Jets: Resistive MHD Nested Grid Simulations
• Magnetic Field Amplification by Small-Scale Dynamo Action: Dependence on Turbulence Models and Reynolds and Prandtl Numbers
• The formation of direct collapse black holes under the influence of streaming velocities
• Simulations of the star-forming molecular gas in an interacting M51-like galaxy
• The Formation of Population III Stars in Gas Accretion Stage: Effects of Magnetic Fields
• Is H3+ cooling ever important in primordial gas?
• Formation sites of Population III star formation: The effects of different levels of rotation and turbulence on the fragmentation behavior of primordial gas
• Merge or survive: Number of Population III stars per minihalo
• The importance of magnetic fields for the initial mass function of the first stars
• Resistive Magnetic Field Generation at Cosmic Dawn
• Saturation of the Turbulent Dynamo
• Magneto-Hydrodynamics of Population III Star Formation
• On the First Generation of Stars
• A moving mesh unstaggered constrained transport scheme for magnetohydrodynamics
• Bipolar planetary nebulae from common envelope evolution of binary stars
• The effect of magnetic fields on the formation of circumstellar discs around young stars
• Fragmentation induced starvation in Population III star formation: a resolution study
• Accretion Phase of Star Formation in Clouds with Different Metallicities
• Protostellar collapse and fragmentation using an MHD GADGET
• The impact of non-ideal magnetohydrodynamic processes on discs, outflows, counter-rotation and magnetic walls during the early stages of star formation
• The Mutual Interaction Between Population III Stars and Self-Annihilating Dark Matter
• Magnetohydrodynamic effect on first star formation: prestellar core collapse and protostar formation

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• Gravitational waves from mergers of Population III binary black holes: roles played by two evolution channels
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• Magnetic fields limit the mass of Population III stars even before the onset of protostellar radiation feedback
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• Revisiting primordial magnetic fields through 21-cm physics: Bounds and forecasts
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• Halo Mergers Enhance the Growth of Massive Black Hole Seeds
• Population III star formation: multiple gas phases prevent the use of an equation of state at high densities
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