Secular evolution of cataclysmic binaries: evolution of the secondary and the period gap

Journal Article · Wed Sep 15 00:00:00 EDT 1982 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/160292· OSTI ID:6850562

D'Antona, F; Mazzitelli, I

The evolution of low-mass main-sequence stars subject to mass loss at constant rates is followed, starting from several initial degrees of hydrogen depletion in the central regions and imposing several different rares of mass loss. During this evolution, stars of progressively smaller mass become fully convective. The behavior of convection along the computed sequences is a function both of the chemical stratification of the star and of the degree of departure from thermal equilibrium. Total mixing for stars initially not largely evolved occurs at Mapprox.0.4 M/sub sun/, and, according to the preceding history of the star, the mixing raises or decreases the /sup 3/He concentration in the core noticeably on a short time scale. The consequent sudden variation of the nuclear luminosity produces a thermal readjustment and a small radius increase or decrease. In more evolved initial models (central hydrogen mass fraction X/sub c/approx.0.30, toal mixing occurs only at Mapprox.0.2 M/sub sun/.

• Research Organization: Osservatorio Astronomico di Roma, Istituto di Astrofisica Spaziale CNR, Frascati
• OSTI ID: 6850562
• Journal Information: Astrophys. J.; (United States), Vol. 260:2
• Country of Publication: United States
• Language: English

Related Subjects

71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
BINARY STARS
STAR EVOLUTION
STAR MODELS
ABUNDANCE
CONVECTION
HELIUM
HYDROGEN
MAIN SEQUENCE STARS
MASS
MIXING
NOVAE
STELLAR WINDS
WHITE DWARF STARS
DWARF STARS
ELEMENTS
ERUPTIVE VARIABLE STARS
FLUIDS
GASES
MATHEMATICAL MODELS
NONMETALS
RARE GASES
STARS
VARIABLE STARS
640102* - Astrophysics & Cosmology- Stars & Quasi-Stellar
Radio & X-Ray Sources