The solution topology of galactic winds

Details The solution topology of galactic winds The solution topology of galactic winds

Jun 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994ap%26ss.216..333p&link_type=abstract

Astrophysics and Space Science, vol. 216, no. 1-2, p. 333-335

Astronomy and Astrophysics

Astrophysics

3

Active Galactic Nuclei, Astronomical Models, Gas Dynamics, Gas Flow, Interstellar Gas, Magnetohydrodynamic Flow, Magnetohydrodynamics, Mass Flow, Star Clusters, Stellar Winds, Conservation Laws, Cooling Flows (Astrophysics), Differential Equations, Equations Of State, Manifolds (Mathematics), Plasma Heating, Topology

Scientific paper

The system of ordinary differential equations derived from the
hydrodynamical equations of a radially symmetric flow has a one
dimensional manifold of critical points if there is mass loading in the
flow or if the heating and cooling rates are taken to be independent of
the thermodynamic variables as is usual.

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