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The Evolution of a Slow Nova Model with a Z = .03 Envelope from Pre-explosion to Extinction

Published online by Cambridge University Press:  12 April 2016

D. Prialnik ,
M.M. Shara  and
G. Shaviv
D. Prialnik
Affiliation:
Department of Physics and Astronomy, Tel Aviv University, Ramat Aviv, Tel Aviv, ISRAEL
M.M. Shara
Affiliation:
Department of Physics and Astronomy, Tel Aviv University, Ramat Aviv, Tel Aviv, ISRAEL
G. Shaviv
Affiliation:
Department of Physics and Astronomy, Tel Aviv University, Ramat Aviv, Tel Aviv, ISRAEL

Abstract

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A model for slow nova explosions is presented. The model consists of a 0.8 Mθ C/0 core and an envelope of 10−4 Mθ with solar composition. The envelope is assumed to have been accreted from a companion. The nuclear runaway produces luminosity close to the Eddington luminosity; this ejects 95% of the envelope. We find

  1. I CNO equilibrium burning on a timescale of 105.5 seconds produces enough energy for mass ejection.

  2. II The rise in luminosity stops close to the Eddington limit and the outer envelope layers accelerate via the continuous action of radiation pressure.

  3. III The mass outflow has two phases: a gentle outflow at the beginning and then a rapid outflow. In both phases we find ṁ ⋍ const., or equivalently, steady state outflow.

  4. IV The nova’s “shut-off” mechanism is the exhaustion of the envelope’s mass. In this “slow nova” model it took about 200 days for 95% of the envelope to be ejected and to leave behing a hot white dwarf.

  5. V The isotope ratios C12/C13, N14/N15 and O16/O17 are in good agreement with observations.

  6. VI The behaviour of LBOL(t) agrees well with observations. Several additional consequences are discussed.

Type
Part II: Cataclysmic Variables
Information
International Astronomical Union Colloquium , Volume 42: The Interaction of Variable Stars with their Environment , 1977 , pp. 346 - 364
Copyright
Copyright © Veröff. Der Remeis-Sterwarte 1977

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