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Cosmic-ray driven dynamo in galactic disks

Published online by Cambridge University Press:  01 November 2008

Michał Hanasz ,
K. Otmianowska-Mazur ,
H. Lesch ,
G. Kowal ,
M. Soida ,
D. Wóltański ,
K. Kowalik ,
R. K. Pawłaszek  and
B. Kulesza-Żydzik
Michał Hanasz
Affiliation:
Centre for Astronomy, Nicholas Copernicus University, PL-87148 Piwnice/Toruń, Poland, [email protected]
K. Otmianowska-Mazur
Affiliation:
Astronomical Observatory, Jagiellonian University, ul. Orla 171, 30-244, Kraków
H. Lesch
Affiliation:
Astronomical Observatory, Munich University, Scheinerstr. 1, D-81679, Germany
G. Kowal
Affiliation:
Astronomical Observatory, Jagiellonian University, ul. Orla 171, 30-244, Kraków Department of Physics and Astronomy, McMaster University, 1280 Main St. W., Hamilton, ON L8S 4M1, Canada.
M. Soida
Affiliation:
Astronomical Observatory, Jagiellonian University, ul. Orla 171, 30-244, Kraków
D. Wóltański
Affiliation:
Centre for Astronomy, Nicholas Copernicus University, PL-87148 Piwnice/Toruń, Poland, [email protected]
K. Kowalik
Affiliation:
Centre for Astronomy, Nicholas Copernicus University, PL-87148 Piwnice/Toruń, Poland, [email protected]
R. K. Pawłaszek
Affiliation:
Centre for Astronomy, Nicholas Copernicus University, PL-87148 Piwnice/Toruń, Poland, [email protected]
B. Kulesza-Żydzik
Affiliation:
Astronomical Observatory, Jagiellonian University, ul. Orla 171, 30-244, Kraków
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Abstract

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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.

Keywords

Galaxies: ISM – magnetic fields – ISM: cosmic rays – magnetic fields – MHD
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S259: Cosmic Magnetic Fields: From Planets, to Stars and Galaxies , November 2008 , pp. 479 - 484
Copyright
Copyright © International Astronomical Union 2009

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