CNO abundances and hydrodynamic models of the nova outburst. II - 1.00 solar mass models with enhanced carbon and oxygen

Details CNO abundances and hydrodynamic models of the nova outburst. II - 1.00 solar mass models with enhanced carbon and oxygen CNO abundances and hydrodynamic models of the nova outburst. II - 1.00 solar mass models with enhanced carbon and oxygen

Aug 1974

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974apjs...28..247s&link_type=abstract

Astrophysical Journal Supplement Series (Supplement no. 261), vol. 28, Aug. 1974, p. 247-270.

Statistics

Computation

132

Abundance, Hydrodynamics, Novae, Stellar Evolution, Stellar Mass Ejection, White Dwarf Stars, Astronomical Models, Carbon, Hydrogen Plasma, Nitrogen, Oxygen, Stellar Envelopes, Thermonuclear Reactions

Scientific paper

Results of a computation of a variety of evolutionary sequences involving thermonuclear runaways in the hydrogen-rich envelopes of 1.00-solar-mass carbon-oxygen white dwarfs. The evidence concerning the location of the outburst in the nova system is reexamined, and it is concluded that the white dwarf is the seat of the outburst. An order-of-magnitude argument is presented which indicates that for a 1.00-solar-mass white dwarf it is impossible to achieve mass ejection without an energy generation of approximately 10 to the 16th ergs/g/sec. A description is given of models with low nuclear enhancements that do not produce an outburst, although their evolution has certain implications for the cause of the dwarf-nova outburst. The results for models that produced a nova outburst are then presented, and on the basis of these results it is found possible to explain continuous ejection, Kukarkin and Parenago's (1934) relationship, and other gross features of the nova phenomena.

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