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Cosmic-ray driven dynamo in galaxies

Published online by Cambridge University Press:  08 June 2011

M. Hanasz ,
D. Wóltanski ,
K. Kowalik  and
H. Kotarba
M. Hanasz
Affiliation:
Centre for Astronomy, Nicolaus Copernicus University, ul. Gagarina 11, PL-87-100 Torun, Poland
D. Wóltanski
Affiliation:
Centre for Astronomy, Nicolaus Copernicus University, ul. Gagarina 11, PL-87-100 Torun, Poland
K. Kowalik
Affiliation:
Centre for Astronomy, Nicolaus Copernicus University, ul. Gagarina 11, PL-87-100 Torun, Poland
H. Kotarba
Affiliation:
University Observatory Munich, Scheinerstr. 1, D-81679 Munich, Germany
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Abstract

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We present recent developments of global galactic-scale numerical models of the Cosmic Ray (CR) driven dynamo, which was originally proposed by Parker (1992). We conduct a series of direct CR+MHD numerical simulations of the dynamics of the interstellar medium (ISM), composed of gas, magnetic fields and CR components. We take into account CRs accelerated in randomly distributed supernova (SN) remnants, and assume that SNe deposit small-scale, randomly oriented, dipolar magnetic fields into the ISM. The amplification timescale of the large-scale magnetic field resulting from the CR-driven dynamo is comparable to the galactic rotation period. The process efficiently converts small-scale magnetic fields of SN-remnants into galactic-scale magnetic fields. The resulting magnetic field structure resembles the X-shaped magnetic fields observed in edge-on galaxies.

Keywords

Galaxies: ISMMagnetic FieldsISM: Cosmic RaysMagnetic FieldsMHD: Dynamos
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S274: Advances in Plasma Astrophysics , September 2010 , pp. 355 - 360
Copyright
Copyright © International Astronomical Union 2011

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