Astronomy and Astrophysics – Astronomy
Scientific paper
May 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...230l..37a&link_type=abstract
Astrophysical Journal, Part 2 - Letters to the Editor, vol. 230, May 15, 1979, p. L37-L40.
Astronomy and Astrophysics
Astronomy
108
Astronomical Models, Gamma Ray Astronomy, Gravitational Collapse, Supernovae, Cobalt Isotopes, Helium, Iron, Light Curve, Nebulae, Neutron Stars, Nickel Isotopes, Positrons, Shock Wave Luminescence, Stellar Evolution, Stellar Mass Ejection
Scientific paper
A theoretical analysis of the light curves of Type I supernovae is presented. A low-mass helium star (helium mass of about 1.5 to 4 solar masses), formed by mass transfer in a binary or by extensive mass loss, undergoes core collapse to form a neutron star. The 'reflected' shock synthesizes and ejects about 0.3 solar mass of Ni-56. The low-mass mantle slows the Ni-56 but allows it to escape. The shock does not give a vigorous display in the visual wavelengths because the envelope is not sufficiently extended to do so. The decay of Ni-56 powers the peak of the light curve; exponential-tail phase is powered by kinetic energy from positron emission by Co-56. The Co-Fe 'core' lights a surrounding, rapidly expanding, He-rich nebula. During the tail phase, the luminosity in gamma-ray lines is about 20 times that observed in the visible, and should be detectable with gamma-ray spectrometers now operational.
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