Mathematics – Logic
Scientific paper
Dec 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...18110212s&link_type=abstract
American Astronomical Society, 181st AAS Meeting, #102.12; Bulletin of the American Astronomical Society, Vol. 24, p.1286
Mathematics
Logic
Scientific paper
The puzzling 1980-81 deep light minimum of PU Vul following its 1977 outburst has been interpreted in terms of a dust condensation model (cf. Men'shchikov et al. 1985, Sov.Astr.Letters 11, 221) and an eclipse of the hot component by the larger M giant (cf. Belyakina et al. 1984, Astr.Ap. 132, L12). Both of these explanations have serious difficulties (cf. Iijima 1989, Astr.Ap. 215, 57). A sequence of quasi-static evolutionary models of a hot, low mass (0.5 Msun) white dwarf accreting H-rich matter at a rate 1 times 10(-8) Msun/yr was generated. The initial model parameters were: Log R (cm) = 9.32, Log Teff = 5.048, Log L(Lsun) = 2.113, Log rho (H shell) = 1.8, Log T (H-shell) = 7.51, Log P (H-shell) = 17.478, epsilon_ {cno} (ergs/g/s) = 1.2 times 10(9) , Log Menv= 3.31 times 10(-4) Msun. This sequence has revealed the occurrence of two successive, closely spaced, hydrogen shell flashes, the second one triggered 21 years after the first one, by the rapid contractional heating of the white dwarf (still burning hydrogen at a much reduced rate) following the partial quenching of the first flash. The morphological behavior of this sequence (but with shortened timescales corresponding to a higher mass accreting degenerate) provides a promising possible explanation for PU Vul's 1980-81 deep light minimum. This work was supported in part by NSF grant AST90-16283 and NASA grant NAG5-1284 to Villanova University.
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