The evolution of cooling flows. I - Self-similar cluster flows

Details The evolution of cooling flows. I - Self-similar cluster flows The evolution of cooling flows. I - Self-similar cluster flows

Jul 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...318...66c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 318, July 1, 1987, p. 66-77.

Astronomy and Astrophysics

Astrophysics

14

Cooling Flows (Astrophysics), Cosmic Gases, Galactic Clusters, Gas Cooling, Gas Density, Intergalactic Media, Magnetohydrodynamic Flow, Radiative Heat Transfer, Astronomical Models, Cosmic Rays, Magnetic Effects, Radiation Pressure, Thermal Instability

Scientific paper

The evolution of a cooling flow from an initial state of hydrostatic equilibrium is studied. If the gravitational potential is that of a singular isothermal sphere, the gas is initially isothermal and the radiative cooling function is a power law of temperature, then the flow is self-similar. Mass removal by thermal instability can be approximately included in the self-similar solutions. The addition of magnetic or cosmic-ray pressure shows that the non-thermal pressure comes to dominate the pressure in the inner parts of the flow, where the density profile is flattened.

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