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Very Deep inside the SN 1987A Core Ejecta: Molecular Structures Seen in 3D
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2017 (English)In: Astrophysical Journal Letters, ISSN 2041-8205, E-ISSN 2041-8213, Vol. 842, no 2, L24Article in journal (Refereed) Published
Abstract [en]

Most massive stars end their lives in core-collapse supernova explosions and enrich the interstellar medium with explosively nucleosynthesized elements. Following core collapse, the explosion is subject to instabilities as the shock propagates outward through the progenitor star. Observations of the composition and structure of the innermost regions of a core-collapse supernova provide a direct probe of the instabilities and nucleosynthetic products. SN 1987A in the Large Magellanic Cloud is one of very few supernovae for which the inner ejecta can be spatially resolved but are not yet strongly affected by interaction with the surroundings. Our observations of SN 1987A with the Atacama Large Millimeter/submillimeter Array are of the highest resolution to date and reveal the detailed morphology of cold molecular gas in the innermost regions of the remnant. The 3D distributions of carbon and silicon monoxide (CO and SiO) emission differ, but both have a central deficit, or torus-like distribution, possibly a result of radioactive heating during the first weeks ("nickel heating"). The size scales of the clumpy distribution are compared quantitatively to models, demonstrating how progenitor and explosion physics can be constrained.

Place, publisher, year, edition, pages
Institute of Physics Publishing , 2017. Vol. 842, no 2, L24
Keyword [en]
hydrodynamics, Instabilities, ISM: supernova remnants, Supernovae: individual (SN 1987A) Supporting material: Animation
National Category
Physical Sciences
Identifiers
URN: urn:nbn:se:kth:diva-216454DOI: 10.3847/2041-8213/aa784cScopus ID: 2-s2.0-85021380728OAI: oai:DiVA.org:kth-216454DiVA: diva2:1162981
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QC 20171205

Available from: 2017-12-05 Created: 2017-12-05 Last updated: 2017-12-05Bibliographically approved

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Larsson, Josefin

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  • apa
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  • en-GB
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  • nn-NB
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Output format
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