Astronomy and Astrophysics – Astrophysics
Scientific paper
Nov 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...310..222p&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 310, Nov. 1, 1986, p. 222-237.
Astronomy and Astrophysics
Astrophysics
130
Astronomical Models, Novae, Stellar Evolution, Abundance, Nuclear Fusion, Stellar Composition, Stellar Envelopes, Stellar Mass Accretion, Stellar Mass Ejection
Scientific paper
The evolution of a classical nova model is followed through accretion, outburst, mass loss, decline, and resumed accretion, leading to a second outburst, by means of an implicit, Lagrangian hydrodynamic code, which includes diffusion (concentration, pressure, and thermal terms), as well as an extensive nuclear reaction network between 28 isotopes of C, N, O, F, Ne, Na, Mg, and Al. The initial model is a 1.25 M_sun; C-O white dwarf (WD) and the accretion rate assumed is 10-11M_sun; yr-1. The accreted matter has normal composition (Z = 0.03). It is found that by the action of diffusion and convection some WD material is mixed into the accreted matter, raising the CNO mass fraction to Z ≈ 0.3. The resulting outburst resembles a fast nova eruption, with a peak bolometric luminosity of 2.9×105L_sun;, t3 = 25 days, an ejected mass of 6.5×10-6M_sun;, and a maximum velocity of 3800 km s-1.
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