Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aas...19915706v&link_type=abstract
American Astronomical Society, 199th AAS Meeting, #157.06; Bulletin of the American Astronomical Society, Vol. 34, p.566
Astronomy and Astrophysics
Astrophysics
Scientific paper
The Classical Nova outburst is a result of a thermonuclear runaway in the accreted hydrogen rich envelope on the white dwarf component of a close binary system. Classical novae participate in the cycle of Galactic chemical evolution in which grains and metal enriched gas in their ejecta, supplementing those of supernovae, AGB stars, and WR stars, are a source of heavy elements for the ISM. Observational studies done over the past 20 years have shown that their ejecta are enriched in material that must have been dredged up from the underlying white dwarf at some time during the runaway. However, it is still unclear as to both when and how white dwarf material is carried up into the accreted material although one-dimensional simulations have shown that a very strong convective region appears during the progress of the runaway. In order to address these questions, we have begun a multidimensional study of the development of the convective region to the surface using the Virginia Hydrodynamics code (VH-1) developed by Blondin and colleagues. Our version of the code includes a realistic (non-polytropic) equation of state, a large nuclear reaction network and thermal diffusion. In the first stages of our investigation, reported here, we compare the results of our one-dimensional calculations with previous studies. In the near future we will extend these studies to two and three dimensions. This work was supported in part by NASA Astrophysical Theory Program grant (NAG5-9263) to ASU.
Hix William Raphael
Starrfield Summer
Vanhala Harri A. T.
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