The Role of Magnetic Fields in Galactic Hydrostatic Equilibrium

Details The Role of Magnetic Fields in Galactic Hydrostatic Equilibrium The Role of Magnetic Fields in Galactic Hydrostatic Equilibrium

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999ptep.proc...98f&link_type=abstract

Plasma Turbulence and Energetic Particles in Astrophysics, Proceedings of the International Conference, Cracow (Poland), 5-10 Se

Astronomy and Astrophysics

Astrophysics

Scientific paper

Hydrostatic equilibrium of the multiphase ISM in the solar vicinity is reconsidered with the regular and turbulent magnetic fields treated separately. For |z| < 1 kpc and |z| > 3-4 kpc, the regular magnetic field strength required to support the gas is consistent with independent estimates provided energy equipartition is maintained between turbulence and random magnetic fields in diffuse phases, but not for the bulk motions of molecular clouds. The layer at 1 < |z| < 3 kpc is overpressured and an outflow at = 50 km{ṡ}s-1 may occur there, driving a Galactic fountain flow. Hydrostatic equilibrium in a warped disc must produce asymmetric density distributions in z, in rough agreement with H I observations in the outer Galaxy.

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