| Issue |
EAS Publications Series
Volume 56, 2012
The Role of the Disk-Halo Interaction in Galaxy Evolution: Outflow vs. Infall?
|
|
|---|---|---|
| Page(s) | 347 - 354 | |
| Section | Modelling the Disk-Halo Interaction in Galaxies | |
| DOI | https://doi.org/10.1051/eas/1256057 | |
| 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 ;
e-mail: mhanasz@astri.uni.torun.pl
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