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Magnetohydrodynamic Simulation of the Evolution of Large-Scale Magnetic Fields in Disk Galaxies

  • Robert C. Bishop (a1), Paul R. Shapiro (a1) and Daniel C. Barnes (a2)

Abstract

The amplification of a seed magnetic field by the hydrodynamic behavior of a disk galaxy is an important and challenging problem. We present our initial work on a numerical simulation of the amplification of such a field to large scales and its subsequent evolution. The computations will be carried out using a 3-D magnetohydrodynamic code.

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Copyright

References

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Barnes, D. C., Bishop, R. C., Milroy, R. D. and Schnack, D. D. (in preparation), “Flexible Semiimplicit Algorithms For Bounded Multi-dimensional MHD Calculations”, in preparation for submission to J. Comp. Phys.
Braginskii, S. I. (1965), “Transport Properties in a Plasma”, in Leontovich, M. A., ed., Reviews of Plasma Physics.
Harned, D. S. and Kerner, J. W. (1985), J. Comp. Phys. 60, 62.
Robert, A. J. (1969), Proc. WMO/IUGG Symp. on Numerical Weather Prediction.
Schnack, D. D., Barnes, D. C., Mikic, Z., Harned, D. S. and Caramana, E. J. (1987), J. Comp. Phys. 70, 330.
Welter, G. L., Perry, J. J. and Kronberg, P. P. (1984), Ap. J. 279, 19.
Wolfe, A M. (1988), in Quasar Absorption Lines: Probes of the Universe , Blades, , et. al, eds.

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