Regular magnetic fields in coronae of spiral galaxies

Details Regular magnetic fields in coronae of spiral galaxies Regular magnetic fields in coronae of spiral galaxies

Sep 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990natur.347...51s&link_type=abstract

Nature (ISSN 0028-0836), vol. 347, Sept. 6, 1990, p. 51-53.

Computer Science

48

Dynamo Theory, Interstellar Magnetic Fields, Spiral Galaxies, Poloidal Flux, Synchrotron Radiation, Turbulent Flow

Scientific paper

The idea that large-scale ordered magnetic fields might reside in the gaseous coronae of spiral galaxies is developed. The partially ionized gas in the coronae is in chaotic motion, both turbulent and convective, and acquires a nonzero mean helicity due to galactic rotation. Differential rotation and this helicity generate a magnetic field with predicted magnitude of about 1 microgauss and with a scale comparable to that of the corona. This field is nearly independent of the disk magnetic field, and a galactic-scale neutral sheet arises about 1 kpc above one side of the disk. At heights of about 3-5 kpc, the poloidal magnetic field component dominates the corona, a result consistent with the observations of polarization in the galaxy NGC4631.

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