Rapid accretion and hibernation in the preoutburst history of classical novae

Statistics – Computation

Scientific paper

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Binary Stars, Stellar Evolution, Stellar Mass Accretion, Cataclysmic Variables, Computational Astrophysics, Stellar Composition, Stellar Luminosity, Thermonuclear Reactions

Scientific paper

The authors outline a model of nova evolution which takes account of varying binary semimajor axes because of nova mass ejection, and secondary heating by the primary during the posteruptive phase. The model predicts that mass transfer should cease a few centuries after eruption, remain off for millennia ("hibernation"), and then resume when angular momentum losses bring the secondary back into contact with its Roche lobe. Numerical simulations have been carried out to study the effects of two high M(10-8M_sun;yr-1) episodes lasting centuries, separated by hibernation times of 0, 103, 104, and 105yr. The models yielded thermonuclear runaways, violent enough to eject mass at typical nova velocities, despite the fact that all accreted mass was deposited at M= 10-8M_sun;yr-1. These models explain the apparent discrepancy between mass accretion observations and the theory of mass accretion onto prenova, and the surprising rarity of novae discovered in surveys.

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