Hydrogen shell flashes in massive accreting white dwarfs

Journal Article · Fri Jun 15 00:00:00 EDT 1979 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/157143· OSTI ID:5983433

Sion, E M; Acierno, M J; Tomczyk, S

The long-term evolution of massive (M>1.1 M/sub sun/) accreting white dwarfs in close binary systems is discussed in the context of several astrophysical problems. The evolution of massive white dwarfs was followed with model calculations. The models have /sup 12/C--/sup 16/O cores and envelopes with composition X=0.7, Z=0.03. The accreted hydrogen-rich matter was assumed to have the same composition as the stellar envelope. A 1.2 M/sub sun/ white dwarf accreting at the rate 1.03 x 10/sup -7/ M/sub sun/ yr/sup -1/ gives rise to repetitive hydrogen shell flashes with an interflash period of 17 years. A 1.2 M/sub sun/ white dwarf accreting at the rate 1.03 x 10/sup -8/ M/sub sun/ yr/sup -1/ has an interflash period of approximately 630 years. A 1.3 M/sub sun/ white dwarf accreting at the rate 2.71 x 10/sup -7/ M/sub sun/ yr/sup -1/ undergoes stable hydrogen burning in a steady state with accretion.The possible relationship of our models to understanding the underlying variability of the blue component of symbiotic variables is discussed. The application of our models to X-ray sources containing massive degenerate dwarfs undergoing rapid accretion is considered.

• Research Organization: Department of Astronomy, Villanova University
• OSTI ID: 5983433
• Journal Information: Astrophys. J.; (United States), Vol. 230:3
• Country of Publication: United States
• Language: English

Related Subjects

71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
WHITE DWARF STARS
STAR MODELS
BINARY STARS
CHEMICAL COMPOSITION
COSMIC X-RAY SOURCES
LUMINOSITY
STAR ACCRETION
STAR EVOLUTION
STEADY-STATE CONDITIONS
COSMIC RAY SOURCES
DWARF STARS
MATHEMATICAL MODELS
OPTICAL PROPERTIES
PHYSICAL PROPERTIES
STARS
640102* - Astrophysics & Cosmology- Stars & Quasi-Stellar
Radio & X-Ray Sources