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The light curve of SN 1987A revisited: Constraining production masses of radioactive nuclides

Seitenzahl, Ivo; Timmes, F X; Magkotsios, Georgios

Description

We revisit the evidence for the contribution of the long-lived radioactive nuclides 44Ti, 55Fe, 56Co, 57Co, and 60Co to the UVOIR light curve of SN 1987A. We show that the V-band luminosity constitutes a roughly constant fraction of the bolometric luminosity between 900 and 1900 days, and we obtain an approximate bolometric light curve out to 4334 days by scaling the late time V-band data by a constant factor where no bolometric light curve data is available. Considering the five most relevant...[Show more]

dc.contributor.authorSeitenzahl, Ivo
dc.contributor.authorTimmes, F X
dc.contributor.authorMagkotsios, Georgios
dc.date.accessioned2015-12-08T22:09:12Z
dc.identifier.issn0004-637X
dc.identifier.urihttp://hdl.handle.net/1885/28926
dc.description.abstractWe revisit the evidence for the contribution of the long-lived radioactive nuclides 44Ti, 55Fe, 56Co, 57Co, and 60Co to the UVOIR light curve of SN 1987A. We show that the V-band luminosity constitutes a roughly constant fraction of the bolometric luminosity between 900 and 1900 days, and we obtain an approximate bolometric light curve out to 4334 days by scaling the late time V-band data by a constant factor where no bolometric light curve data is available. Considering the five most relevant decay chains starting at 44Ti, 55Co, 56Ni, 57Ni, and 60Co, we perform a least squares fit to the constructed composite bolometric light curve. For the nickel isotopes, we obtain best fit values of M(56Ni) = (7.1 ± 0.3) × 10 -2 M ⊙ and M(57Ni) = (4.1 ± 1.8) × 10-3 M ⊙. Our best fit 44Ti mass is M(44Ti) = (0.55 ± 0.17) × 10-4 M ⊙, which is in disagreement with the much higher (3.1 ± 0.8) × 10-4 M ⊙ recently derived from INTEGRAL observations. The associated uncertainties far exceed the best fit values for 55Co and 60Co and, as a result, we only give upper limits on the production masses of M(55Co) < 7.2 × 10-3 M ⊙ and M(60Co) < 1.7 × 10-4 M ⊙. Furthermore, we find that the leptonic channels in the decay of 57Co (internal conversion and Auger electrons) are a significant contribution and constitute up to 15.5% of the total luminosity. Consideration of the kinetic energy of these electrons is essential in lowering our best fit nickel isotope production ratio to [57Ni/56Ni] = 2.5 ± 1.1, which is still somewhat high but is in agreement with gamma-ray observations and model predictions.
dc.publisherIOP Publishing
dc.rightsAuthor/s retain copyright
dc.sourceAstrophysical Journal, The
dc.titleThe light curve of SN 1987A revisited: Constraining production masses of radioactive nuclides
dc.typeJournal article
local.description.notesImported from ARIES
local.identifier.citationvolume792
dc.date.issued2014
local.identifier.absfor020100 - ASTRONOMICAL AND SPACE SCIENCES
local.identifier.ariespublicationu4830877xPUB61
local.type.statusPublished Version
local.contributor.affiliationSeitenzahl, Ivo, College of Physical and Mathematical Sciences, ANU
local.contributor.affiliationTimmes, F X, Arizona State University
local.contributor.affiliationMagkotsios, Georgios, The Joint Institute for Nuclear Astrophysics
local.bibliographicCitation.issue10
local.bibliographicCitation.startpage1
local.bibliographicCitation.lastpage7
local.identifier.doi10.1088/0004-637X/792/1/10
local.identifier.absseo970102 - Expanding Knowledge in the Physical Sciences
dc.date.updated2015-12-08T07:23:03Z
local.identifier.scopusID2-s2.0-84906243671
dcterms.accessRightsOpen Access
CollectionsANU Research Publications

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