Time-independent models of white dwarfs accreting mass

Details Time-independent models of white dwarfs accreting mass Time-independent models of white dwarfs accreting mass

Dec 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975a%26a....45..411s&link_type=abstract

Astronomy and Astrophysics, vol. 45, no. 2, Dec. 1975, p. 411-416.

Astronomy and Astrophysics

Astrophysics

25

Astronomical Models, Mass Flow Rate, Novae, Stellar Mass, White Dwarf Stars, Helium, Hydrogen, Mass Transfer, Stellar Envelopes, Stellar Evolution, Stellar Structure, Time Dependence

Scientific paper

Simplified models of 1 solar mass and 1.39 solar mass white dwarfs accreting matter have been obtained. These models consist of envelopes, stationary shell source regions and highly degenerate isothermal cores. The accreted matter flows from the surface through the hydrogen- and helium-burning shells into the core. The range of mass-flow rates for which hydrogen- and helium-burning shell sources may be stationary and the time scales of their formation have been determined. The thermal and pulsational stability of each model must be checked to ensure that the model represents a realistic process. Each of them, however, may be used as an initial condition to follow the evolution of instabilities in the hydrogen and helium shell sources.

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