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Main Sequence Structures Including The Overadiabatic CM Convection Model

Published online by Cambridge University Press:  12 April 2016

Italo Mazzitelli  and
Francesca D’Antona
Italo Mazzitelli
Affiliation:
Istituto di Astrofisica Spaziale, Frascati, Italy
Francesca D’Antona
Affiliation:
Osservatorio Astronomico di Roma, Monte Porzio, Italy

Abstract

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We computed the main sequence structure of masses from 2 to 0.7 M⊙ for two choices of helium (Y) and metal (Z) mass fractions. Models are given for solar composition (Y=0.285, Z=0.018) and for a composition appropriate to a younger population I (Y=0.32, Z=0.03). We took particular care both in the choice of the most recent opacities presently available and in the treatment of the input physics and numerics (see also D’Antona et al, 1992).

Opacities from Rogers and Iglesias (1992) were adopted where available, complemented with those by Kurucz (1991) at T≤10000 K and, elsewhere, by the Los Alamos opacities (Huebner et al. 1977). The equation of state by Mihalas et al. (1988) was used at ρ ≤ 0.01, and elsewhere the relation P = P(ρ,T) was taken from Magni and Mazzitelli (1979), while the adiabatic gradient was obtained from a Saha type e.o.s..

Type
V. The changing interior
Information
International Astronomical Union Colloquium , Volume 137: Inside the Stars , 1993 , pp. 457 - 460
Copyright
Copyright © Astronomical Society of the Pacific 1993

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