On the composition dependence of thermonuclear runaway models for the recurrent nova U Scorpii

Details On the composition dependence of thermonuclear runaway models for the recurrent nova U Scorpii On the composition dependence of thermonuclear runaway models for the recurrent nova U Scorpii

Jan 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...324..345t&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 324, Jan. 1, 1988, p. 345-354.

Astronomy and Astrophysics

Astrophysics

23

Novae, Stellar Composition, Stellar Envelopes, Stellar Mass Ejection, Stellar Models, Thermonuclear Reactions, White Dwarf Stars, Heavy Nuclei, Helium, Hydrogen, Stellar Luminosity, Stellar Mass Accretion

Scientific paper

We report the results of numerical simulations of thermonuclear runaways leading to nova-type outbursts in accreted shells on white dwarfs of mass 1.38 Msun. We assume an accretion rate M =1018 g s-1 onto a white dwarf of intrinsic luminosity 0.1 Lsun and explore the consequences of variations in the composition of the envelope matter. Calculations have been performed, specifically, for hydrogen to helium ratios H/He = 3:1, 2:1, 1:1, 1:2, and 1:8 by mass, for an assumed mass fraction of heavy nuclei compatible with solar abundances. Optically bright outbursts are obtained only for matter of initial composition H/He> 1. In contrast, observations of the ejecta of the recurrent nova U Sco suggest it to be hydrogen depleted: He/H ˜ 1-2 by number. The implications of these results for thermonuclear runaway models for recurrent novae are discussed.

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