On the amplification of large-scale magnetic fields in spiral galaxies by galactic winds

Details On the amplification of large-scale magnetic fields in spiral galaxies by galactic winds On the amplification of large-scale magnetic fields in spiral galaxies by galactic winds

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...400..484s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 400, no. 2, p. 484-501.

Astronomy and Astrophysics

Astrophysics

9

Interstellar Magnetic Fields, Magnetohydrodynamic Turbulence, Spiral Galaxies, Stellar Winds, Magnetic Field Configurations, Plasma Dynamics, Turbulent Diffusion, Volterra Equations

Scientific paper

The regenerative amplification of large-scale magnetic fields in a turbulent disk due to shear in large-scale plasma motions is demonstrated. An axisymmetric 3D velocity field exhibiting radial shear of the axial component and axial shear of the radial component plus differential rotation may support a 3D nonaxisymmetric large-scale magnetic field. Diffusion of the axial and/or radial components of field toward the disk midplane makes regenerative action possible for exclusively outward directed winds. The shear of the wind components provides the critical coupling mechanisms between the radial and axial components of the large-scale magnetic field, permitting growth under diverse conditions. This is qualitatively shown by a spatially integrated dynamic model and quantitatively supported by specific examples of plasma motions in a local model solved by numerical methods. An example of a possible regenerative mechanism due to nonaxisymmetric plasma motions representative of a propagating spiral density wave has also been discussed.

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