On a thermonuclear origin for the 1980-81 deep light minimum of the symbiotic nova PU VUL

Details On a thermonuclear origin for the 1980-81 deep light minimum of the symbiotic nova PU VUL On a thermonuclear origin for the 1980-81 deep light minimum of the symbiotic nova PU VUL

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aj....106..298s&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 106, no. 1, p. 298-300.

Mathematics

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Hot Stars, Novae, Stellar Evolution, Symbiotic Stars, Thermonuclear Explosions, White Dwarf Stars, Light Curve, Morphology, Steady State, Stellar Mass Accretion, Stellar Models

Scientific paper

The puzzling 1980-81 deep light minimum of the symbiotic nova PU Vul is discussed in terms of a sequence of quasi-static evolutionary models of a hot, 0.5 solar mass white dwarf accreting H-rich matter at a rate 1 x 10 exp -8 solar mass/yr. On the basis of the morphological behavior of the models, it is suggested that the deep light minimum of PU Vul could have been the result of two successive, closely spaced, hydrogen shell flashes on an accreting white dwarf whose core thermal structure and accreted H-rich envelope was not in a long-term thermal 'cycle-averaged' steady state with the rate of accretion.

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