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Gamma-ray line measurements from supernova explosions

Published online by Cambridge University Press:  17 October 2017

Roland Diehl Open the ORCID record for Roland Diehl [Opens in a new window]
Roland Diehl*
Affiliation:
Max Planck Institut für extraterrestrische Physik Giessenbachstr. 1, D-85748 Garching, Germany email: rod@mpe.mpg.de
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Abstract

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Gamma ray lines are expected to be emitted as part of the afterglow of supernova explosions, because radioactive decay of freshly synthesised nuclei occurs. Significant radioactive gamma ray line emission is expected from 56Ni and 44Ti decay on time scales of the initial explosion (56Ni, τ ~days) and the young supernova remnant (44Ti,τ ~90 years). Less specific, and rather informative for the supernova population as a whole, are lessons from longer lived isotopes such as 26Al and 60Fe. From isotopes of elements heavier than iron group elements, any interesting gamma-ray line emission is too faint to be observable. Measurements with space-based gamma-ray telescopes have obtained interesting gamma ray line emissions from two core collapse events, Cas A and SN1987A, and one thermonuclear event, SN2014J. We discuss INTEGRAL data from all above isotopes, including all line and continuum signatures from these two objects, and the surveys for more supernovae, that have been performed by gamma ray spectrometry. Our objective here is to illustrate what can be learned from gamma-ray line emission properties about the explosions and their astrophysics.

Keywords

gamma rays: observations(stars:) supernovae: general(stars:) supernovae: individual (Cas A, SN1987A, SN2014J)(ISM:) supernova remnantsGalaxy: kinematics and dynamics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S331: Supernova 1987A:30 years later - Cosmic Rays and Nuclei from Supernovae and their aftermaths , February 2017 , pp. 157 - 163
Copyright
Copyright © International Astronomical Union 2017 

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