Other
Scientific paper
Mar 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aipc..402..203s&link_type=abstract
Astrophysical implications of the laboratory study of presolar materials. AIP Conference Proceedings, Volume 402, pp. 203-234 (
Other
19
Novae, Dwarf Novae, Recurrent Novae, And Other Cataclysmic Variables, Nucleosynthesis In Novae, Supernovae, And Other Explosive Environments, Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages, Interstellar Dust Grains, Diffuse Emission, Infrared Cirrus
Scientific paper
The nova outburst is a consequence of the accretion of hydrogen-rich material onto a white dwarf (WD) in a close binary system. The strong degeneracy of the massive WD prevents the expansion of the gas and drives the temperatures in the nuclear burning region to values exceeding 108K under all circumstances. As a result, a major fraction of the CNO nuclei in the envelope are transformed into β-decay nuclei. The energy released from the decay of these nuclei is responsible for ejecting 10-5Msolar to 10-4Msolar of gas at high velocities. A major fraction of novae in outburst are observed to form dust in the ejected matter and we review the infrared (IR) observations which reveal the onset and evolution of this dust formation phase. We discuss the characteristics of nova dust and show that it may be the most interesting dust produced by any astrophysical object. IR observations show, in addition, that novae appear capable of condensing dust with at least four different chemical and mineral compositions. We argue that the class of ONeMg novae may form dust grains that carry the Ne-E and 26Mg anomalies observed in meteoritic grains. We also report on the results of new calculations of thermonuclear runaways on both carbon-oxygen and oxygen-neon-magnesium white dwarfs using our one-dimensional, fully implicit, hydrodynamic stellar evolution code that includes a large nuclear reaction network. We have updated both the nuclear reaction network and the nuclear reaction rates. Our results show that the changes in the reaction rates and opacities produce quantitative changes with respect to our earlier studies. The causes are (1) that the new opacities are larger than those we previously used, which results in less mass being accreted onto the white dwarf, and (2) that the protoncapture reaction rates for some of the intermediate mass nuclei near 26Al have increased so that the evolution to higher mass nuclei is enhanced.
Gehrz Robert D.
Starrfield Summer
Truran Jame. W.
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