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- W4281787453 abstract "Abstract We present a model for one cycle of a classical nova outburst based on a self-consistent wind mass loss accelerated by the gradient of radiation pressure, i.e., so-called optically thick winds. Evolution models are calculated by a Henyey code for a 1.0 $M_{odot }$ white dwarf with a mass-accretion rate of 5 × 10−9 $M_{odot }$ yr−1. The outermost part of the hydrogen-rich envelope is connected to a steadily moving envelope where optically thick winds occur. We confirm that no internal shock waves occur at thermonuclear runaway. The wind mass-loss rate reaches a peak of 1.4 × 10−4 $M_{odot }$ yr−1 at the epoch of the maximum photospheric expansion, where the photospheric temperature decreases to log Tph (K) = 3.90. Almost all of the accreted mass is lost in the wind. The nuclear energy generated in hydrogen burning is lost in a form of photon emission (64%), gravitational energy (lifting up the wind matter against gravity, 35%), and the kinetic energy of the wind (0.23%). A classical nova should be very bright in a far-UV (100–300 Å) band for one day just after the onset of thermonuclear runaway (∼ 25 d before the optical maximum). In the decay phase of the nova outburst, the envelope structure is very close to that of a steady-state solution." @default.
- W4281787453 created "2022-06-13" @default.
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- W4281787453 date "2022-07-18" @default.
- W4281787453 modified "2023-10-14" @default.
- W4281787453 title "Physics of nova outbursts: A theoretical model of classical nova outbursts with self-consistent wind mass loss" @default.
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- W4281787453 doi "https://doi.org/10.1093/pasj/psac051" @default.
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