Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...267..779s&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 267, April 15, 1983, p. 779-794.
Astronomy and Astrophysics
Astrophysics
31
Hubble Constant, Nuclear Models, Stellar Models, Supernovae, Black Body Radiation, Gamma Rays, Light Curve, Neutron Stars, Nickel Isotopes, Opacity, Positrons, Radioactivity, Stellar Evolution
Scientific paper
In recent years, considerable progress has been made toward understanding Type I supernovae within the context of radioactive energy input. Much effort has gone into determining the peak magnitude of the supernovae, particularly in the B-band, and its relation to the Hubble constant. If the distances inferred for Type I events are at all accurate, and/or the Hubble constant has a value near 50 km per s per Mpc, it is clear that models must reach a peak magnitude approximately -20 in order to be consistent. The present investigation is concerned with models which achieve peak magnitudes near this value and contain 0.8 solar mass of Ni-56. The B-band light curve declines much more rapidly after peak than the bolometric light curve. The mass and velocity of Ni-56 (at least for the A models) are within the region defined by Axelrod (1980) for configurations which produce acceptable spectra at late times. The models are consistent with the absence of a neutron star after the explosion. There remain, however, many difficult problems.
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