Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...259..244i&link_type=abstract
Astrophysical Journal, Part 1, vol. 259, Aug. 1, 1982, p. 244-266.
Astronomy and Astrophysics
Astrophysics
246
Stellar Mass Accretion, Stellar Models, White Dwarf Stars, Helium, Hydrogen, Novae, Stellar Envelopes, Stellar Evolution, Stellar Luminosity
Scientific paper
Properties of white dwarfs which are accreting hydrogen-rich matter at rates in the range 1.5 x 10 to the -9th to 2.5 x 10 to the -7th solar mass/yr are investigated in several approximations. Steady-burning models, in which matter is processed through nuclear-burning shells as rapidly as it is accreted, provide a framework for understanding the properties of models in which thermal pulses induced by hydrogen burning and helium burning are allowed to occur. In these latter models, the underlying carbon-oxygen core is chosen to be in a cycle-averaged steady state with regard to compressional heating and neutrino losses. Several of these models are evolved in the quasi-static approximation. Combining results obtained in the steady-burning approximation with those obtained in the quasi-static approximation, expressions are obtained for estimating, as functions of accretion rate and white dwarf mass, the thermal pulse recurrence period and the duration of hydrogen-burning phases.
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