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The Half-Life of Titanium 44 and SN 1987A

Published online by Cambridge University Press:  25 May 2016

Yuko S. Mochizuki  and
Shiomi Kumagai
Yuko S. Mochizuki
Affiliation:
The Institute of Physical and Chemical Research (RIKEN) Hirosawa 2-1, Wako, Saitama 351-01, JAPAN
Shiomi Kumagai
Affiliation:
Department of Physics, College of Science and Technology, Nihon University Kanda-Surugadai 1-8, Chiyoda-ku, Tokyo 101, JAPAN

Extract

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The radioactive isotopes, such as 44Ti and 56Ni, are synthesized as a result of rapid nucleosynthesis in supernova explosions. The gamma-ray photons coming out from the decay sequence of 44Ti is now a strong candidate to explain the the late light curve of SN 1987A. It is noted here that the energy release from the 44Ti decay depends strongly on its half-life. However, the published values for 44Ti half-life display a large spread, ranging from ~ 35 to ~ 68 years. In this paper (Kumagai et al. 1997; see also Kumagai et al. 1993), we discuss the value of the half-life by comparing the theoretical light curves and the observations in SN 1987A. The unestablished half-life value is related to the ratio of the abundance of 44Ti to that of 56Ni.

Type
Session 1: Plasma and Fresh Nucleosynthesis Phenomena
Information
Symposium - International Astronomical Union , Volume 188: The Hot Universe , 1998 , pp. 241 - 242
Copyright
Copyright © Kluwer 1998 

References

Kumagai, S., Mochizuki, Y.S., Nomoto, K., and Tanihata, I. (1997) in preparation Google Scholar
Kumagai, S., Nomoto, K., Shigeyama, T., Hashimoto, M., and Itoh, M. (1993) “Detection of 57Co γ rays from SN 1987A and prospect of X-ray observations of the pulsar with ASCA”, Astron. & Astrophys. , 273, pp. 153–159 Google Scholar
Suntzeff, N.B. (1997) in SN1987A: Ten Years After, The Fifth CTIO/ESO/LCO Workshop, eds. Phillips, M.M. and Suntzeff, N.B., in press Google Scholar