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Date and Time of the Query: 2019-06-26 T12:02:28 PDT
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For refcode 1994ApJ...426L..89K:
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1994ApJ...426L..89K EVIDENCE FOR ^56^Ni - ^56^Co - ^56^Fe DECAY IN TYPE Ia SUPERNOVAE MARC J. KUCHNER AND ROBERT P. KIRSHNER Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; kuchner@cfa.harvard.edu, kirshner@cfa.harvard.edu PHILIP A. PINTO Steward Observatory, University of Arizona, Tucson, AZ 85721; pinto%aristarchus@as.ariaona.edu AND BRUNO LEIBUNDGUT European Southern Observatory, Karl-Schwarzschild-Strasse 2,85748 Garching bei Munchen, Germany; bleibund@eso.org Received 1993 December 30; accepted 1994 March 1 ABSTRACT In the prevailing picture of Type Ia supernovae (SN Ia), their explosive burning produces ^56^Ni, and the radioactive decay chain ^56^Ni - ^56^Co - ^56^Fe 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 ^56^Fe/^56^Co abundance ratio follows from ^56^Ni - ^56^Co - ^56^Fe 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 ^56^Ni, just as predicted by a wide range of models for SN Ia explosions. Subject headings: supernovae: general
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