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Non Crystallized Regions of White Dwarfs. Thermodynamics. Opacity. Turbulent Convection

Published online by Cambridge University Press:  12 April 2016

I. Mazzitelli
I. Mazzitelli*
Affiliation:
Istituto di Astrofisica Spaziale. Consiglio Nazionalt delle Ricerche, C.P. 67, 00044 Frascati.Italy

Abstract

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The evolution of White Dwarf stars along their cooling sequences is governed not only by their thermal content, but also by the rate at which heat flows through the external, partially degenerate and non-isothermal layers. In particular, cooling is found to be largely influenced both by the optical atmosphere, and by the convective envelope. The first one, in fact, determines the internal density stratification, down to the point at which electron degeneracy takes over, while the second one affects the temperature stratification in the same layers. The reliability of the present generation of models of White Dwarf envelopes is discussed, on the grounds of the main physical inputs (thermodynamics, opacity, convection theory), for both H-rich and He-rich surface chemical compositions. The conclusion is that, below Log L/L⊙ ≤ −3, we can build little more than test models

Type
Reviews
Information
International Astronomical Union Colloquium , Volume 147: The Equation of State in Astrophysics , 1994 , pp. 144 - 160
Copyright
Copyright © Cambridge University Press 1994

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