Abstract
Havazelet and Barkat (1979) have shown that at the stage of evolution of intermediate-mass stars which is characterized by the presence of a double burning shell (H, He) on top of a mostly degenerate C-O core, whose mass is m(c), the stellar luminosity (l, in solar units) depends almost only on m(c). Paczynski (1970) obtained a linear luminosity-core mass relationship. The present investigation is concerned with a suitable theoretical explanation regarding the existence and form of the l-m(c) relations. An approach is shown for deriving the existence of these relations under a basic set of assumptions together with the homology assumption. It is assumed that the star has a core of mass m(c) which resembles a classical white dwarf. It has a thin burning shell which surrounds the core. The luminosity in the transition zone is assumed to be constant and equal to the local radiative luminosity l.
Original language | American English |
---|---|
Pages (from-to) | 356-360 |
Number of pages | 5 |
Journal | Astrophysical Journal |
Volume | 268 |
Issue number | 1 |
DOIs | |
State | Published - 1983 |