Magnetic fields in the formation of the first stars.--II Results

  title={Magnetic fields in the formation of the first stars.--II Results},
  author={Athena Stacy and Christopher F. McKee and Aaron Lee and Richard Klein and Pak Shing Li},
Beginning with cosmological initial conditions at z = 100, we simulate the effects of magnetic fields on the formation of Population III stars and compare our results with the predictions of Paper I. We use gadget-2 to follow the evolution of the system while the field is weak. We introduce a new method for treating kinematic fields by tracking the evolution of the deformation tensor. The growth rate in this stage of the simulation is lower than expected for diffuse astrophysical plasmas, which… 

Fundamental scales in the kinematic phase of the turbulent dynamo

The turbulent dynamo is a powerful mechanism that converts turbulent kinetic energy to magnetic energy. A key question regarding the magnetic field amplification by turbulence, is, on what scale,

Ion alfvén velocity fluctuations and implications for the diffusion of streaming cosmic rays

The interstellar medium (ISM) of star-forming galaxies is magnetized and turbulent. Cosmic rays (CRs) propagate through it, and those with energies from ∼ GeV − TeV are likely subject to the

Exponentially Amplified Magnetic Field Eliminates Disk Fragmentation around Population III Protostars

One critical remaining issue that is unclear in the initial mass function of the first (Population III) stars is the final fate of secondary protostars that formed in the accretion disk—specifically,



2011b) that the minimum resolution

  • 2011

On the other hand, numerical simulations have found CΓ ≪ 1, presumably because of the greater importance of dissipation

  • 2002

Magnetic fields in first star formation–II

  • MNRAS,
  • 2017

2004)’s simulation included explicit viscosity and resistivity whereas Federrath et al. (2011a)’s simulation was an ideal MHD simulation with numerical viscosity and resistivity

  • Since Federrath et al
  • 2011

where r is the distance to the particle a from a given point in the computational box. The contribution of a particle a to the density at a given point is

  • 2001

2011a) explored the properties of small-scale

  • 2011

Magnetic fields in first star formation–II

  • 2011

They found Γ ≃ vL/L for subsonic, solenoidally driven turbulence, which corresponds to CΓ ≃ Re = 0.026. Compressively driven turbulence was much less effective at driving a dynamo

  • 2011

Wesenberg M

  • Journal Comp. Phys
  • 2002

In a set of ideal MHD simulations with 1283 grid cells, Federrath et al. (2011a) explored the properties of small-scale dynamos as a function of the Mach number of the turbulence

  • 2011