The Thermal State of Accreting White Dwarfs Undergoing Classical Novae

@inproceedings{Townsley2003TheTS,
  title={The Thermal State of Accreting White Dwarfs Undergoing Classical Novae},
  author={Dean M. Townsley and Lars Bildsten},
  year={2003}
}
White dwarfs experience a thermal renaissance when they rec ive mass from a stellar companion in a binary. For accretion rates< 10M⊙ yr−1, the freshly accumulated hydrogen/helium envelope ignite s in a thermally unstable manner that results in a classical novae (CN) outbu rst and ejection of material. We have undertaken a theoretical study of the impact of the accumulating envelop n the thermal state of the underlying white dwarf (WD). This has allowed us to find the equilibrium WD core tempe… 
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References

SHOWING 1-4 OF 4 REFERENCES
AIP CONF PROC
Cambridge Astrophysics Series
  • Cambridge Astrophysics Series
  • 1995
Soviet Astron
  • Soviet Astron
  • 1980