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dc.contributor.authorLarsson, Josefin
dc.contributor.authorFransson, Claes
dc.contributor.authorKjaer, Karina
dc.contributor.authorJerkstrand, Anders
dc.contributor.authorKirshner, Robert P.
dc.contributor.authorLeibundgut, Bruno
dc.contributor.authorLundqvist, Peter
dc.contributor.authorMattila, Seppo
dc.contributor.authorMcCray, Richard
dc.contributor.authorSollerman, Jesper
dc.contributor.authorSpyromilio, Jason
dc.contributor.authorWheeler, J. Craig
dc.date.accessioned2019-09-25T14:12:34Z
dc.date.issued2013
dc.identifier.citationLarsson, Josefin, Claes Fransson, Karina Kjaer, Anders Jerkstrand, Robert P. Kirshner, Bruno Leibundgut, Peter Lundqvist, et al. 2013. “THE MORPHOLOGY OF THE EJECTA IN SUPERNOVA 1987A: A STUDY OVER TIME AND WAVELENGTH.” The Astrophysical Journal 768 (1): 89. https://doi.org/10.1088/0004-637x/768/1/89.
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.urihttp://nrs.harvard.edu/urn-3:HUL.InstRepos:41399807*
dc.description.abstractWe present a study of the morphology of the ejecta in Supernova 1987A based on images and spectra from the Hubble Space Telescope (HST) as well as integral field spectroscopy from VLT/SINFONI. The HST observations were obtained between 1994 and 2011 and primarily probe the outer H-rich zones of the ejecta. The SINFONI observations were obtained in 2005 and 2011 and instead probe the [Si I]+[Fe II] emission from the inner regions. We find a strong temporal evolution of the morphology in the HST images, from a roughly elliptical shape before similar to 5000 days, to a more irregular, edge-brightened morphology with a "hole" in the middle thereafter. This transition is a natural consequence of the change in the dominant energy source powering the ejecta, from radioactive decay before similar to 5000 days to X-ray input from the circumstellar interaction thereafter. The [Si I]+[Fe II] images display a more uniform morphology, which may be due to a remaining significant contribution from radioactivity in the inner ejecta and the higher abundance of these elements in the core. Both the Ha and the [Si I]+[Fe II] line profiles show that the ejecta are distributed fairly close to the plane of the inner circumstellar ring, which is assumed to define the rotational axis of the progenitor star. The Ha emission extends to higher velocities than [Si I]+[Fe II], as expected from theoretical models. There is no clear symmetry axis for all the emission. Instead, we find that the emission is concentrated to clumps and that the emission is distributed somewhat closer to the ring in the north than in the south. This north-south asymmetry may be partially explained by dust absorption. We compare our results with explosion models and find some qualitative agreement, but note that the observations show a higher degree of large-scale asymmetry.
dc.language.isoen_US
dc.publisherAmerican Astronomical Society
dash.licenseLAA
dc.titleThe Morphology of the Ejecta in Supernova 1987a: A Study Over Time and Wavelength
dc.typeJournal Article
dc.description.versionVersion of Record
dc.relation.journalThe Astrophysical Journal
dash.depositing.authorKirshner, Robert P.::0f07c3b6230f5e5a42326bcba12a1795::600
dc.date.available2019-09-25T14:12:34Z
dash.workflow.comments1Science Serial ID 99663
dc.identifier.doi10.1088/0004-637X/768/1/89
dash.source.volume768;1
dash.source.page89


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