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X-Ray and Gamma-Ray Emission from Core-collapse Supernovae: Comparison of Three-dimensional Neutrino-driven Explosions with SN 1987A
KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics. The Oskar Klein Centre, AlbaNova, SE-106 91 Stockholm, Sweden.
KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics. The Oskar Klein Centre, AlbaNova, SE-106 91 Stockholm, Sweden.ORCID iD: 0000-0003-0065-2933
Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan..
Stockholm Univ, Oskar Klein Ctr, Dept Astron, AlbaNova, SE-10691 Stockholm, Sweden..
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2019 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 882, no 1, article id 22Article in journal (Refereed) Published
Abstract [en]

During the first few hundred days after the explosion, core-collapse supernovae (SNe) emit down-scattered X-rays and gamma-rays originating from radioactive line emissions, primarily from the Ni-56 -> Co-56 -> Fe-56 chain. We use supernova (SN) models based on three-dimensional neutrino-driven explosion simulations of single stars and mergers to compute this emission and compare the predictions with observations of SN 1987A. A number of models are clearly excluded, showing that high-energy emission is a powerful way of discriminating between models. The best models are almost consistent with the observations, but differences that cannot be matched by a suitable choice of viewing angle are evident. Therefore, our self-consistent models suggest that neutrino-driven explosions are able to produce, in principle, sufficient mixing, although remaining discrepancies may require small changes to the progenitor structures. The soft X-ray cutoff is primarily determined by the metallicity of the progenitor envelope. The main effect of asymmetries is to vary the flux level by a factor of similar to 3. For the more asymmetric models, the shapes of the light curves also change. In addition to the models of SN 1987A, we investigate two models of SNe II-P and one model of a stripped-envelope SN IIb. The Type II-P models have observables similar to those of the models of SN 1987A, but the stripped-envelope SN model is significantly more luminous and evolves faster. Finally, we make simple predictions for future observations of nearby SNe.

Place, publisher, year, edition, pages
IOP PUBLISHING LTD , 2019. Vol. 882, no 1, article id 22
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:kth:diva-259428DOI: 10.3847/1538-4357/ab3395ISI: 000483094200004OAI: oai:DiVA.org:kth-259428DiVA, id: diva2:1353908
Conference
AYTON DD, 1991, ASTROPHYSICAL JOURNAL, V375, P221 jcha Ondrej, 2015, ASTROPHYSICAL JOURNAL, V806, rrison Fiona A., 2013, ASTROPHYSICAL JOURNAL, V770, ade W, 1934, PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA, V20, P259 nka Hans-Thomas, 2016, ANNUAL REVIEW OF NUCLEAR AND PARTICLE SCIENCE, VOL 66, V66, P341 naud N, 2004, ASTROPARTICLE PHYSICS, V21, P201, AYTON DD, 1969, ASTROPHYSICAL JOURNAL, V155, P75, AYTON DD, 1974, ASTROPHYSICAL JOURNAL, V188, P155 zdnyakov L.A., 1983, Astrophysics and Space Physics Reviews, V2, P189
Note

QC 20190924

Available from: 2019-09-24 Created: 2019-09-24 Last updated: 2019-09-24Bibliographically approved

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