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Theoretical light curve for the recurrent nova RS Ophiuchi - Determination of the white dwarf mass, composition, and distance
Kato, Mariko
AA(Pennsylvania State University, University Park; Illinois, University, Urbana)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 369, March 10, 1991, p. 471-474. (ApJ Homepage)
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NASA/STI Keywords:
Light Curve, Novae, Ophiuchi Clouds, Stellar Composition, Stellar Mass Accretion, White Dwarf Stars, Binary Stars, Heavy Elements, Nuclear Transformations, Stellar Models
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Sequences of steady mass-loss solutions are constructed for the envelopes on a white dwarf with mass 1.33, 1.35, 1.36, 1.37, and 1.377 solar mass as models of the decay phase of novae. The envelopes are assumed to have a uniform chemical composition with X = 0.73, 0.6, 0.52, 0.44, 0.33, and 0.11 for hydrogen and Z = 0.02 for heavy elements by weight. An excellent agreement with the observed light curves of UV and optical is obtained in the models with a white dwarf mass of 1.36 solar mass with hydrogen content X = 0.52, and 1.37 solar mass with X = 0.6. The distance of RS Oph is obtained to be 1.6 kpc from the comparison between the theoretical and observed light curves. The success of this wind model is a strong indication from the theoretical point of view that RS Oph is a thermonuclear runaway event.

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