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Classical Nova Evolution: Clues from Soft X-ray Emission

  • James Macdonald
Part of the Astrophysics and Space Science Library book series (ASSL, volume 208)

Abstract

Multi-wavelength observations have shown that, after optical decline, the stellar remnants of classical nova outbursts evolve at constant, near-Eddington, bolometric luminosity to high effective temperature (> 2105 K), before turning off. Here we briefly review the observations of classical novae in this phase of evolution, and discuss what the soft X-ray observations tell us about the mass of the underlying white dwarf and the rate of mass change due to stellar winds and accretion from the stellar companion.

Keywords

White Dwarf Orbital Separation Envelope Material Nuclear Burning Classical Nova 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© Kluwer Academic Publishers 1996

Authors and Affiliations

  • James Macdonald
    • 1
  1. 1.Department of Physics and AstronomyUniversity of DelawareNewarkUSA

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