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TNR on Top of Accreting WDs: 2-D Simulations

Published online by Cambridge University Press:  12 April 2016

S. A. Glasner ,
E. Livne  and
J. W. Truran
S. A. Glasner
Affiliation:
Racah Institute of Physics, The Hebrew University, Jerusalem, Israel
E. Livne
Affiliation:
Racah Institute of Physics, The Hebrew University, Jerusalem, Israel
J. W. Truran
Affiliation:
University of Chicago, Lab. forAstrophysics and Space Research, Enrico Fermi Institute, Chicago, IL 60637, USA

Extract

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Spherically symmetric models for classical novae as thermonuclear run-aways (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.

Type
Novae & Symbiotic Stars
Information
International Astronomical Union Colloquium , Volume 158: Cataclysmic Variables and Related Objects , 1996 , pp. 299 - 300
Copyright
Copyright © Kluwer 1996

References

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