The evolution of a classical nova model through a complete cycle

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Abstract
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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