EAS Publications Series
Volume 56, 2012The Role of the Disk-Halo Interaction in Galaxy Evolution: Outflow vs. Infall?
|Page(s)||347 - 354|
|Section||Modelling the Disk-Halo Interaction in Galaxies|
|Published online||17 September 2012|
Miguel A. de Avillez (ed)
EAS Publications Series, 56 (2012) 347–354
Incorporating Cosmic Rays In Local And Global Models Of Disk-Halo Interaction
1 Centre for Astronomy, Nicholas Copernicus University, Toruń, Poland ;
2 Astronomical Observatory, Jagiellonian University, Kraków, Poland
3 Astronomical Observatory, Munich University, Munich, Germany
4 Department of Physics and Astronomy, McMaster University, Hamilton, Canada
We present new developments on the cosmic-ray driven, galactic dynamo, modeled by means of direct, resistive CR–MHD simulations, performed with ZEUS and PIERNIK codes. The dynamo action, leading to the amplification of large–scale galactic magnetic-fields on galactic rotation timescales, appears as a result of galactic differential rotation, buoyancy of the cosmic-ray component and resistive dissipation of small–scale turbulent magnetic-fields. Our new results include demonstration of the global–galactic dynamo action driven by cosmic-rays supplied in supernova remnants. An essential outcome of the new series of global galactic dynamo models is the equipartition of the gas turbulent energy with magnetic-field energy and cosmic-ray energy, in saturated states of the dynamo on large galactic scales.
© EAS, EDP Sciences, 2012