EDP Sciences
Free Access
Volume 435, Number 2, May IV 2005
Page(s) 385 - 395
Section Astrophysical processes
DOI https://doi.org/10.1051/0004-6361:20042451
Published online 29 April 2005

A&A 435, 385-395 (2005)
DOI: 10.1051/0004-6361:20042451

Self-gravitational adaptive mesh magnetohydrodynamics with the NIRVANA code

U. Ziegler

Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany
    e-mail: uziegler@aip.de

(Received 29 November 2004 / Accepted 21 January 2005 )

I present a new version of the NIRVANA code capable for the simulation of multi-scale self-gravitational magnetohydrodynamics problems in three space dimensions employing the technique of adaptive mesh refinement. The building blocks of NIRVANA are (i) a fully conservative, divergence-free Godunov-type central scheme for the solution of the equations of magnetohydrodynamics; (ii) a block-structured mesh refinement algorithm which automatically adds and removes elementary grid blocks whenever necessary to achieve adequate resolution and; (iii) an adaptive mesh Poisson solver based on multigrid philosophy which incorporates the so-called elliptic matching condition to keep the gradient of the gravitational potential continous at fine/coarse mesh interfaces. In this paper I give an overview of the basic numerical ideas standing behind NIRVANA and apply the code to the problem of protostellar core collaps and fragmentation.

Key words: magnetohydrodynamics (MHD) -- stars: formation -- methods: numerical -- ISM: magnetic fields

© ESO 2005

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