Other
Scientific paper
Jan 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994phdt.........7y&link_type=abstract
PhD Dissertation, Oklahoma Univ. Oklahoma City, OK United States
Other
4
Light Curve, Supernovae, Stellar Evolution, Stellar Mass Ejection, Stellar Envelopes, Stellar Cores, Nickel Isotopes, Stellar Mass, Stellar Magnitude
Scientific paper
Numerical supernova light curves are calculated from various model progenitor stars. The model progenitor stars have main sequence masses above 10 M(solar mass) which are believed to undergo core collapse and envelope ejection. Two light curve projects have been conducted and four individual SNe have been investigated. The largest project is a parameter study of progenitor stars with 6 M(solar mass) cores and various envelopes. Five parameters that effect the light curve of type 2 supernovae are examined; the ejected mass, the progenitor radius, the explosion energy, the Ni-56 mass, and the extent of Ni-56 mixing. The primary parameters that are of greatest importance to the light curve shape and absolute magnitude are the progenitor radius, total mass, and Ni-56 mass. The secondary parameters which influence the light curve to a lesser degree are found to be the explosion energy, Ni-56 mixing, and the He core mass. The light curves are plotted on an absolute magnitude scale to be easily compared to observations. The model photospheric temperature and photospheric velocity are presented which is useful for comparison to model and observed spectra. It is shown that the light curve shape and absolute magnitude is unique when considering large variations in the parameters, however small changes of the parameters can be reconciled. The Ni diffusion wave and the recombination of He produce a prominent secondary peak found in all calculations. The feature is predicted to be reduced with compositional mixing, both H-He and Ni-56. An auxiliary project investigated the influence of the He core mass while fixing the 5 parameters. It is shown that the He core mass is not an important parameter affecting the light curve. The individual SNe studied are SNe 1987A, 1984L, 199SJ, and 1994I. Parameters and limits of parameters are given for each supernova. Future work includes fitting other observed light curves and obtaining individual parameter values. Compiling these values into distribution functions will show how widely different or similar Type 2 supernovae are.
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