Self-similar collapse and accretion of radiative gas

Details Self-similar collapse and accretion of radiative gas Self-similar collapse and accretion of radiative gas

Sep 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995mnras.276..133b&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 276, Issue 1, pp. 133-166.

Astronomy and Astrophysics

Astronomy

20

Gravitation, Hydrodynamics, Stars: Formation

Scientific paper

The hydrodynamics of spherically symmetric radiative gas is discussed. Self-similar solutions are obtained for situations where the total emissivity epsilon of the gas has a power-law dependence on the density and temperature, epsilon~rho^alphaT^4+beta, in an optically thin medium. A perfect gas equation of state is used throughout. The flows have uniform density and contract uniformly initially. The region of uniform density becomes ever smaller with time, and gives way to power-law radial profiles. For each pair alpha and beta, there may exist three types of flows. Flows of the first type are far from dynamical equilibrium, and have gas converging steadily to the origin. These solutions develop strong velocity fields and supersonic motion. These are found for alpha, beta such that 1/21 and zero velocity; solutions are given for 18 different pairs of alpha and beta. Outflowing envelopes cause the appearance of a `ring' in the luminosity profile, which expands about the central mass. When the outflow is such that the gas leaves the central region, we find no solution except when beta=1-3alpha and with 4/3

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