The luminosity core mass relation - why and how

Y Tuchman, A Glasner, Z Barkat

Research output: Contribution to journalArticlepeer-review


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 languageAmerican English
Pages (from-to)356-360
Number of pages5
JournalAstrophysical Journal
Issue number1
StatePublished - 1983


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