A model for winds from galactic disks.
Abstract
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.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- April 1978
- DOI:
- 10.1086/156008
- Bibcode:
- 1978ApJ...221..105B
- Keywords:
-
- Galactic Radiation;
- Galactic Structure;
- Hydrodynamic Equations;
- Plasmas (Physics);
- Spiral Galaxies;
- Coronas;
- Disks (Shapes);
- Gas Flow;
- Gravitational Fields;
- Astrophysics;
- Galactic Winds:Models;
- Galactic Winds:Spiral Galaxies;
- Galaxies: Structure