A model for winds from galactic disks

Details A model for winds from galactic disks A model for winds from galactic disks

Apr 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...221..105b&link_type=abstract

Astrophysical Journal, Part 1, vol. 221, Apr. 1, 1978, p. 105-113.

Physics

25

Galactic Radiation, Galactic Structure, Hydrodynamic Equations, Plasmas (Physics), Spiral Galaxies, Coronas, Disks (Shapes), Gas Flow, Gravitational Fields

Scientific paper

A hydrodynamic model is constructed to represent a wind originating in the disk of a spiral galaxy. The gas flow is assumed to be steady, nondissipative, axisymmetric, and (to simplify the calculations) self-similar, scaling in radius. Various heating processes are represented by a pressure-density relation which is isothermal near the disk and adiabatic far from the disk. Wind solutions are found for a range of values of initial parameters in the disk. In a regime where the self-similarity might be expected to be valid, scaling parameters can be chosen which are reasonable for a large spiral galaxy with a hot, tenuous corona.

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