Incorporation of cosmic ray transport into the ZEUS MHD code

Free access article

Issue		A&A Volume 412, Number 2, December III 2003


Page(s)		331 - 339
Section		Cosmology
DOI		http://dx.doi.org/10.1051/0004-6361:20031433

A&A 412, 331-339 (2003)
DOI: 10.1051/0004-6361:20031433

Application for studies of Parker instability in the ISM

M. Hanasz¹ and H. Lesch²

¹ Torun Centre for Astronomy, Nicholas Copernicus University, 87148 Piwnice/Torun, Poland
e-mail: mhanasz@astri.uni.torun.pl
² University Observatory, München University, Scheinerstr. 1, 81679, Germany and Center for Interdisciplinary Plasma Science (CIPS)
e-mail: lesch@usm.uni-muenchen.de

(Received 16 June 2003 / Accepted 9 September 2003 )

Abstract
We present a numerical algorithm for the incorporation of the active cosmic ray transport into the ZEUS-3D magnetohydrodynamical code. The cosmic ray transport is described by the diffusion-advection equation. The applied form of the diffusion tensor allows for anisotropic diffusion of cosmic rays along and across the magnetic field direction, which is controlled by two parameters: the parallel and perpendicular diffusion coefficients. The implemented numerical algorithm is tested by comparison of the diffusive transport of cosmic rays to analytical solutions of the diffusion equation. Our method is numerically stable for a wide range of diffusion coefficients, including the realistic values inferred from the observational data for the Milky Way of about $6 \times 10^{28}~{\rm cm}^2\,{\rm s}^{-1}$ . The presented algorithm is applied for exemplary simulations of the Parker instability triggered by cosmic rays injected by a single SN remnant.

Key words: ISM: magnetic fields -- ISM: cosmic rays

Offprint request: M. Hanasz, mhanasz@astri.uni.torun.pl

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