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TNR on Top of Accreting WDS: 2-D Simulations

  • S. A. Glasner
  • E. Livne
  • J. W. Truran
Part of the Astrophysics and Space Science Library book series (ASSL, volume 208)

Abstract

Spherically symmetric models for classical novae as thermonuclear runaways (TNR) of hydrogen-rich, accreted, envelopes on top of cold white dwarfs (WD) are in very good agreement with observations (Starrfield, Sparks & Truran 1974, 1985; Prialnik, Shara & Shaviv 1978; Prialnik 1986; MacDonald 1980). Multi-dimensional investigations are needed since the burning rate is very sensitive to the temperature and small fluctuations in temperature can lead to large differences between the flash times of different points on the burning shell; these differences can be much larger than the rise time of the nova light curve. Convection is assumed to be the mechanism that couples the burning process at different points in the shell so that the overall phenomena is spherically symmetric.

Keywords

Burning Rate White Dwarf Convective Cell Subsonic Flow Cataclysmic Variable 
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.

References

  1. Livne, E., 1993, Ap. J., 412, 634ADSCrossRefGoogle Scholar
  2. MacDonald, J., 1980, MNRAS, 191, 933ADSGoogle Scholar
  3. Prialnik, D., Shara, M.M., Shaviv, G., 1978, A&A, 62, 339ADSGoogle Scholar
  4. Prialnik, D., 1986, Ap. J., 310, 222ADSCrossRefGoogle Scholar
  5. Starrfield, S., Sparks, W.M., Truran, J.W., 1974, Ap. J. Supp., 28, 247 Starrfield, S., Sparks, W.M., Truran, J.W., 1985, Ap. J., 291, 136ADSCrossRefGoogle Scholar

Copyright information

© Kluwer Academic Publishers 1996

Authors and Affiliations

  • S. A. Glasner
    • 1
  • E. Livne
    • 1
  • J. W. Truran
    • 2
  1. 1.Racah Institute of PhysicsThe Hebrew UniversityJerusalemIsrael
  2. 2.Lab. for Astrophysics and Space Research, Enrico Fermi InstituteUniversity of ChicagoChicagoUSA

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