Optically thick winds: How is the mass flux determined?

Details Optically thick winds: How is the mass flux determined? Optically thick winds: How is the mass flux determined?

May 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...445..411g&link_type=abstract

The Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 445, no. 1, p. 411-414

Astronomy and Astrophysics

Astrophysics

Mass Flow, Mass Flow Rate, Novae, Optical Thickness, Stellar Envelopes, Stellar Mass Ejection, Stellar Winds, Acoustic Velocity, Equations Of Motion, Hydrodynamics, Luminosity, Momentum

Scientific paper

Expanding envelopes of compact objects that possess a buring region at the base of the envelope are commonly observed and modeled. In many cases, such as the late stages of classical nova, the expanding envelope develops into a stationary, optically thick wind of matter escaping from the star. In the usual theoretical formalism there is one more unknown than equations, with closure being obtained by the requirement that the solution pass through the singularity at the sonic point. It is shown analytically that the mass flux, which is one of the unknowns, is almost completely determined by the physical conditions near the base of the envelope just above the burning zone. The sonic point closure relation determines whether the expanding solution can develop into a wind solution. For a given core mass the range of possible wind solutions is an outcome of the great sensitivity of the mass flux to the inner luminosity. Solutions determined through numerical integrations are shown to lie entirely within the narrow analytic boundaries.

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