Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...237l..81c&link_type=abstract
Astrophysical Journal, Part 2 - Letters to the Editor, vol. 237, May 1, 1980, p. L81-L85. Research supported by the U.S. Departm
Astronomy and Astrophysics
Astrophysics
121
Gamma Rays, Radioactive Decay, Stellar Luminosity, Supernovae, Beta Particles, Light Curve, Monte Carlo Method, Nickel Isotopes, Positrons, Stellar Models
Scientific paper
The luminosity of type I supernovae is recalculated, and the energy deposition by both gamma rays and positrons is determined using a numerical Monte Carlo program. Three independent physical phenomena are considered: the diffusive release of thermal radiation that determines the height and width of the optical peak; the initial fast decay of the optical peak by a factor of roughly 100 as determined by the progressive transparency to gamma rays, and the apparent 56 day half-life that results from the progressive escape of the positron fraction of the 77 day Co-56 decay. To obtain agreement with observations, each phenomenon requires that the expanding nebula be described by a single relation yielding a value of 0.22 plus or minus 0.05 for the product of the ejected mass (in solar masses), and the expansion velocity (in units of 10 to the 9th cm/s) taken to the -2nd power. It is concluded that the type I supernova light curve with its exponential tail is well explained by the radioactive decay of Ni-56.
Colgate Sterling A.
Kriese John T.
Petschek Albert G.
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