Effects of drag luminosity in the common envelope phase of slow novae

Statistics – Computation

Scientific paper

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Binary Stars, Main Sequence Stars, Novae, Stellar Envelopes, Stellar Luminosity, White Dwarf Stars, Computational Astrophysics, Density Distribution, Stellar Mass, Stellar Models, Stellar Winds

Scientific paper

The present study examines the effects of the drag luminosity during the decay phase of slow novae under the assumption of spherical symmetry for two systems consisting of a 0.9-solar-mass white dwarf and a 0.2-solar mass main-sequence companion, and of a 0.6-solar-mass white dwarf and a 0.2-solar-mass main-sequence companion. The 0.6-solar-mass white dwarf has a more massive envelope than that of the 0.9-solar-mass white dwarf, and its density is much higher than that of the 0.9-solar-mass case, because the frictional energy generation is proportional to the density of material at the companion orbits. It is also found that no optically thick wind occurs, mainly because the gravity of the companion suppresses the wind. As a result, the evolution time scale of the decay phase is not drastically changed for slow novae when the frictional process is included.

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