Magnetic fields during high redshift structure formation

D. R.G. Schleicher, M. Latif, J. Schober, W. Schmidt, S. Bovino, C. Federrath, J. Niemeyer, R. Banerjee, R. S. Klessen

Research output: Contribution to journalArticlepeer-review

9 Citations (Scopus)


We explore the amplification of magnetic fields in the high-redshift Universe. For this purpose, we perform high-resolution cosmological simulations following the formation of primordial halos with ~ ⊙ 107 M, revealing the presence of turbulent structures and complex morphologies at resolutions of at least 32 cells per Jeans length. Employing a turbulence subgrid-scale model, we quantify the amount of unresolved turbulence and show that the resulting turbulent viscosity has a significant impact on the gas morphology, suppressing the formation of low-mass clumps. We further demonstrate that such turbulence implies the efficient amplification of magnetic fields via the small-scale dynamo. We discuss the properties of the dynamo in the kinematic and non-linear regime, and explore the resulting magnetic field amplification during primordial star formation. We show that field strengths of ~ 10-5 G can be expected at number densities of ~ 5 cm-3.

Original languageEnglish
Pages (from-to)531-536
Number of pages6
JournalAstronomische Nachrichten
Issue number6
Publication statusPublished - Jul 2013
Externally publishedYes


  • Cosmology: theory
  • Galaxies: formation
  • Magnetic fields
  • Turbulence

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science


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