The vertical structure of the galactic gaseous disk and its relation to the dynamo problem.

Details The vertical structure of the galactic gaseous disk and its relation to the dynamo problem. The vertical structure of the galactic gaseous disk and its relation to the dynamo problem.

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...311..451f&link_type=abstract

Astronomy and Astrophysics, v.311, p.451-455

Astronomy and Astrophysics

Astrophysics

9

Magnetohydrodynamics (Mhd), Turbulence, Ism: Magnetic Fields, General, Galaxy: Structure

Scientific paper

Galaxy-wide lower limits for the α- and η-coefficients of the turbulent EMF have been obtained combining the empirically found global density distribution of interstellar matter with that minimal turbulent pressure necessary to prevent onset of Parker instability (cf. Bloemen). The criterion used is that delineated by Lachieze-Rey et al.. Upper limits for α and η result from identifying the total internal pressure, following the assumption of hydrostatical equilibrium. The correlation time, τ_corr_, scale like the local hydrostatic time-scale.

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