Computer Science
Scientific paper
Jul 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998egdg.conf..171v&link_type=abstract
"Dynamics of Galaxies and Galactic Nuclei, An International Workshop of the SFB 328 "Evolution of Galaxies" held at the ITA Nove
Computer Science
Scientific paper
A fully three-dimensional MHD kinematic model is applied to simulate the evolution of a large-scale magnetic field in barred and spiral galaxies. As input parameters we use time dependent velocity fields resulted from self-consistent 3D N-body calculations of galactic dynamics. Our present project analyses mainly the influence of the gas flows in non-axisymmetric gravitational disturbances (like spiral arms and bar) onto magnetic field behaviour. The magnetic field is found to evolve towards structures resembling dynamical spiral arms and bars, however its distribution is often much more complicated than the velocity field itself. Furthermore we find that regions with field reversals in the disk appear due to velocity changes in dynamical resonances, like the corotation radius, of non-axisymmetric structures.
Lesch Harald
Otmianowska-Mazur Katarzyna
von Linden Susanne
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