Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...426l..89k&link_type=abstract
Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 426, no. 2, p. 89-92
Astronomy and Astrophysics
Astrophysics
27
Cobalt Isotopes, Iron Isotopes, Nickel Isotopes, Radioactive Decay, Supernovae, Astronomical Photometry, Astronomical Spectroscopy, Nebulae
Scientific paper
In the prevailing picture of Type Ia supernovae (SN Ia), their explosive burning produces Ni-56, and the radioactive decay chain Ni-56 yields Co-56 yields Fe-56 powers the subsequent emission. We test a central feature of this theory by measuring the relative strengths of a (Co III) emission feature near 5900 A and a (Fe III) emission feature near 4700 A. We measure 38 spectra from 13 SN Ia ranging from 48 to 310 days after maximum light. When we compare the observations with a simple multilevel calculation, we find that the observed Fe/Co flux ratio evolves as expected when the Fe-56/Co-56 abundance ratio follows from Ni-56 yields Co-56 yields Fe-56 decay. From this agreement, we conclude that the cobalt and iron atoms we observe through SN Ia emission lines are produced by the radioactive decay of Ni-56, just as predicted by a wide range of models for SN Ia explosions.
Kirshner Robert P.
Kuchner Marc J.
Leibundgut Bruno
Pinto Philip A.
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