Amplification of Galactic Magnetic Fields by the Cosmic-Ray Driven Dynamo

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dc.contributor.author Hanasz, Michał
dc.contributor.author Kowal, Grzegorz
dc.contributor.author Otmianowska-Mazur, Katarzyna
dc.contributor.author Lesch, Harald
dc.date.accessioned 2012-12-19T09:06:13Z
dc.date.available 2012-12-19T09:06:13Z
dc.date.issued 2004-02-27
dc.identifier.citation Astrophys.J. 605 (2004) L33-L36
dc.identifier.other doi:10.1086/420697
dc.identifier.uri http://repozytorium.umk.pl/handle/item/249
dc.description.abstract We present the first numerical model of the magnetohydrodynamical cosmic-ray (CR) driven dynamo of the type proposed by Parker (1992). The driving force of the amplification process comes from CRs injected into the galactic disk in randomly distributed spherical regions representing supernova remnants. The underlying disk is differentially rotating. An explicit resistivity is responsible for the dissipation of the small-scale magnetic field component. We obtain amplification of the large-scale magnetic on a timescale 250 Myr.
dc.language.iso eng
dc.relation.uri http://arxiv.org/abs/astro-ph/0402662
dc.rights info:eu-repo/semantics/openAccess
dc.subject Astrophysics
dc.title Amplification of Galactic Magnetic Fields by the Cosmic-Ray Driven Dynamo
dc.type info:eu-repo/semantics/article

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