DETECTION OF SPECTRAL EVOLUTION IN THE BURSTS EMITTED DURING THE 2008–2009 ACTIVE EPISODE OF SGR J1550−5418

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dc.citation.firstpage150
dc.citation.journalTitleThe Astrophysical Journalen_US
dc.citation.lastpage161
dc.citation.volumeNumber755en_US
dc.contributor.authorVon Kienlin, Andreas
dc.contributor.authorGruber, David
dc.contributor.authorKouveliotou, Chryssa
dc.contributor.authorGranot, Jonathan
dc.contributor.authorBaring, Matthew G.
dc.contributor.authorGogus, Ersin
dc.contributor.authorHuppenkothen, Daniela
dc.contributor.authorKaneko, Yuki
dc.contributor.authorLin, Lin
dc.contributor.authorWatts, Anna L.
dc.contributor.authorBhat, Narayana P.
dc.contributor.authorGuiriec, Sylvain
dc.contributor.authorVan Der Horst, Alexander J.
dc.contributor.authorBissaldi, Elisabetta
dc.contributor.authorGreiner, Jochen
dc.contributor.authorMeegan, Charles A.
dc.contributor.authorPaciesas, William S.
dc.contributor.authorPreece, Robert D.
dc.contributor.authorRau, Arne
dc.contributor.publisherThe American Astronomical Societyen_US
dc.date.accessioned2013-03-13T19:00:21Z
dc.date.available2014-03-19T05:10:04Z
dc.date.issued2012
dc.description.abstractIn early 2008 October, the soft gamma repeater SGR J1550−5418 (1E 1547.0−5408, AX J155052−5418, PSR J1550−5418) became active, emitting a series of bursts which triggered the Fermi Gamma-ray Burst Monitor (GBM) after which a second especially intense activity period commenced in 2009 January and a third, less active period was detected in 2009 March–April. Here, we analyze the GBM data for all the bursts from the first and last active episodes. We performed temporal and spectral analysis for all events and found that their temporal characteristics are very similar to the ones of other SGR bursts, as well the ones reported for the bursts of the main episode (average burst durations ∼170 ms). In addition, we used our sample of bursts to quantify the systematic uncertainties of the GBM location algorithm for soft gamma-ray transients to 8◦. Our spectral analysis indicates significant spectral evolution between the first and last set of events. Although the 2008 October events are best fitted with a single blackbody function, for the 2009 bursts an optically thin thermal bremsstrahlung is clearly preferred.We attribute this evolution to changes in the magnetic field topology of the source, possibly due to effects following the very energetic main bursting episode.en_US
dc.embargo.terms1 yearen_US
dc.identifier.citationVon Kienlin, Andreas, Gruber, David, Kouveliotou, Chryssa, et al.. "DETECTION OF SPECTRAL EVOLUTION IN THE BURSTS EMITTED DURING THE 2008–2009 ACTIVE EPISODE OF SGR J1550−5418." <i>The Astrophysical Journal,</i> 755, (2012) 150-161. http://dx.doi.org/10.1088/0004-637X/755/2/150.*
dc.identifier.doihttp://dx.doi.org/10.1088/0004-637X/755/2/150en_US
dc.identifier.urihttps://hdl.handle.net/1911/70566
dc.language.isoengen_US
dc.subject.keywordpulsarsen_US
dc.subject.keywordindividual (SGR J1550−5418, 1E 1547.0−5408, PSR J1550−5418) – starsen_US
dc.subject.keywordneutron – X-raysen_US
dc.subject.keywordburstsen_US
dc.titleDETECTION OF SPECTRAL EVOLUTION IN THE BURSTS EMITTED DURING THE 2008–2009 ACTIVE EPISODE OF SGR J1550−5418en_US
dc.typeJournal articleen_US
dc.type.dcmiTexten_US
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