Generation of dynamo magnetic fields in protoplanetary and other astrophysical accretion disks

Details Generation of dynamo magnetic fields in protoplanetary and other astrophysical accretion disks Generation of dynamo magnetic fields in protoplanetary and other astrophysical accretion disks

Aug 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...331..416s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 331, Aug. 1, 1988, p. 416-434.

Statistics

Computation

52

Accretion Disks, Computational Astrophysics, Dynamo Theory, Protostars, Stellar Magnetic Fields, Stellar Mass Accretion, Astronomical Models, Computational Grids, Planetary Nebulae, Pre-Main Sequence Stars

Scientific paper

Many astrophysical objects have disklike structures; these objects range from protostellar/protoplanetary accretion disks to high-energy accretion disks around compact objects, and galaxies. In this paper a computational method is presented for treating the generation of dynamo magnetic fields in astrophysical disks. The numerical difficulty of handling the boundary conditions at infinity in the cylindrical disk geometry is overcome by embedding the disk in a spherical computational space and matching the solutions to analytically tractable spherical functions in the surrounding space. The method is applied to calculate the lowest lying dynamo normal modes for a "thick" astrophysical disk. The generated modes are all oscillatory and spatially localized. The authors discuss the potential implications of these initial results for the properties of dynamo magnetic fields in real astrophysical disks.

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