Physics
Scientific paper
Jul 1976
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976natur.262..118r&link_type=abstract
Nature, vol. 262, July 8, 1976, p. 118-120.
Physics
7
Half Life, Luminous Intensity, Radioactive Decay, Supernovae, White Dwarf Stars, Decay Rates, Electron Density (Concentration), Light Curve, Stellar Mass
Scientific paper
Evidence supporting the hypothesis proposed by Leventhal and McCall (1975), which suggests the beta-decay chain Ni-56 to Co-56 to Fe-56 as a source of supernova luminosity, is presented. In this model, a Type I supernova produces a white dwarf containing about 0.2 solar masses of Ni-56. The high electron densities encountered by the bare nuclei at the interior of the white dwarf produce an enhancement of the decay rates. The supernova luminosity is given as a function of the half lives of the steep early portion and the flat, later portion of the light curve (T1 and T2, respectively) and of parameters whose values depend on the initial amount of Ni-56, the energy releases per decay of Ni-56 and Co-56, and the values of T1 and T2. The values of these parameters were determined for 15 Type I light curves. The relationship between T1 and T2 for these curves was found to be in good agreement with that predicted by the radioactive decay hypothesis. Results further imply an upper mass limit of about 0.4 solar masses for white dwarfs produced.
Leventhal Marvin
McCall S. L.
Rust Bert W.
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