The evolution of a fast nova model with a Z = 0.03 envelope from pre-explosion to decline

Details The evolution of a fast nova model with a Z = 0.03 envelope from pre-explosion to decline The evolution of a fast nova model with a Z = 0.03 envelope from pre-explosion to decline

Feb 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979a%26a....72..192p&link_type=abstract

Astronomy and Astrophysics, vol. 72, no. 1-2, Feb. 1979, p. 192-203.

Astronomy and Astrophysics

Astrophysics

58

Novae, Stellar Envelopes, Stellar Evolution, Stellar Models, White Dwarf Stars, Abundance, Convection, Stellar Luminosity, Stellar Magnitude, Stellar Mass, Stellar Mass Ejection, Thermonuclear Explosions

Scientific paper

The limits of the applicability of the slow nova model suggested by Prialnik et al. (1978) are investigated. A model for fast nova explosions is presented which consists of a 1.25-solar mass C/O core and an envelope of 0.00001 solar mass with Z = 0.03. The envelope is assumed to have been accreted from a companion. The explosion ejects 50% of the envelope at a luminosity close to the Eddington luminosity. It is found that: (1) the nuclear runaway is halted by the conversion of all CNO nuclei into beta-unstable isotopes. It occurs away from the core-envelope interface and subsequently a burning front recedes through the envelope, supplying more nuclear energy; (2) mass loss is driven by radiation pressure and an approximately constant mass-loss rate. A small part of the mass is ejected at a very high velocity, while the rest has relatively low velocities; (3) the nova 'shut-off' mechanism is the extinction of nuclear burning due to fast expansion about 30 d after the outburst; and (4) the postnova object is a hot white dwarf radiating in the far-UV at a rate close to the Eddington luminosity.

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