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3–D Models of Galaxy Magnetic Fields with Spiral Shocks

Published online by Cambridge University Press:  19 July 2016

J. Panesar  and
A.H. Nelson
J. Panesar
Affiliation:
Physics Department University of Wales College of Cardiff Cardiff CF1 3TH, U.K.
A.H. Nelson
Affiliation:
Physics Department University of Wales College of Cardiff Cardiff CF1 3TH, U.K.

Extract

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We report here some preliminary results of 3–D numerical simulations of an α–ω dynamo in galaxies with differential rotation, small–scale turbulence, and a shock wave induced by a stellar density wave. We obtain the magnetic field from the standard dynamo equation, but include the spiral shock velocity field from a hydrodynamic simulation of the gas flow in a gravitational field with a spiral perturbation (Johns and Nelson, 1986).

Type
4. Magnetohydrodynamics of Galactic Magnetic Fields
Information
Symposium - International Astronomical Union , Volume 140: Galactic and Intergalactic Magnetic Fields , 1990 , pp. 133 - 134
Copyright
Copyright © Kluwer 1990 

References

Johns, T.C. and Nelson, A.H. (1986) ‘Global Simulations of Gas Flow in Disc Galaxies’, M.N.R.A.S. 220, 165.Google Scholar