Ni-56 and the light curve of Type I supernova
Abstract
Consideration is given to the explanation for the luminosity decay characteristics of a Type I supernova after maximum in terms of the radioactive decay of Ni-56 ejected in the explosion. It is noted that such an explanation requires a transparency function of 0.22 expressed in units of solar masses and 10 to the 9th cm/sec to account for the light curve, and a minimum mass of Ni-56 to explain the peak and near peak luminosities. Considerations of existing UV and IR observations and the theoretical consequences of radioactive energy loss by work on the expanding nebula imply that the conversion of trapped radioactive decay energy to optical energy is nearly 100% efficient, and therefore gamma ray and beta(+) escape must be the most likely energy loss. For the case of supernova 1972e, the above arguments imply a transparency function of 0.22 with a Ni-56 mass of 0.25 or 0.4 solar masses for distances of 3.2 or 4 Mpc, respectively.
- Publication:
-
Texas Workshop on Type I Supernovae
- Pub Date:
- 1980
- Bibcode:
- 1980tsup.work...42C
- Keywords:
-
- Light Curve;
- Nickel Isotopes;
- Radioactive Decay;
- Stellar Spectra;
- Supernovae;
- Infrared Astronomy;
- Stellar Luminosity;
- Ultraviolet Astronomy;
- Astrophysics