Other
Scientific paper
Aug 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997phdt.........4v&link_type=abstract
Thesis (PHD). ARIZONA STATE UNIVERSITY , Source DAI-B 58/10, p. 5439, Apr 1998, 157 pages.
Other
Stellar Evolution
Scientific paper
Since astronomers have only known about the existence of oxygen-magnesium-neon (ONeMg) novae for the last decade or so, little work has been done on them as a group. It is the purpose of this work to study three fast ONeMg novae: V838 Nova Herculis 1991, V693 Nova Corona Austrinae 1981, and Nova LMC 1990#1. Each of these novae have been studied in detail and a comparison of the results is provided in order to better understand ONeMg novae as a class. These analyses have provided values of the elemental abundances, ejection velocities, ejected masses, white dwarf masses, maximum outburst luminosities, and white dwarf turn-off time for each of these novae. The results of this study can be used in many ways to help further the understanding of novae and stellar evolution. The elemental abundances that have been determined can be used as input to theoretical hydrodynamic models. This will provide better constraints on the models in order to determine the energetics of the outburst and the mass of the underlying white dwarf, properties which are difficult to obtain observationally. The determination of the abundances will also help determine the contribution of fast ONeMg novae to the heavy element content of the interstellar medium (ISM). In particular, with the abundance results, the mass fraction of 26Al and 22Na in the novae ejecta can be estimated. These estimates will help to determine if novae are important for galactic nucleosynthesis. Analysis of Nova LMC 1990#1 provides the means to compare Galactic with extragalactic novae. The results for Nova LMC 1990#1, combined with results from other Large Magellanic Cloud novae, can be used to calibrate the luminosities of (and therefore distances to) Galactic novae. This calibration may allow a better determination of the fast end of the absolute-magnitude decay-rate relationship (or perhaps develop a separate relationship for these objects). A tight, well-defined relationship is crucial for novae to be reliable standard candles.
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