X-Ray Burst and Persistent Emission Properties of the Magnetar SGR 1830-0645 in Outburst

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dc.citation.articleNumber136
dc.citation.journalTitleThe Astrophysical Journal
dc.citation.volumeNumber924
dc.contributor.authorYounes, George
dc.contributor.authorHu, Chin-Ping
dc.contributor.authorBansal, Karishma
dc.contributor.authorRay, Paul S.
dc.contributor.authorPearlman, Aaron B.
dc.contributor.authorKirsten, Franz
dc.contributor.authorWadiasingh, Zorawar
dc.contributor.authorGöğüş, Ersin
dc.contributor.authorBaring, Matthew G.
dc.contributor.authorEnoto, Teruaki
dc.contributor.authorArzoumanian, Zaven
dc.contributor.authorGendreau, Keith C.
dc.contributor.authorKouveliotou, Chryssa
dc.contributor.authorGüver, Tolga
dc.contributor.authorHarding, Alice K.
dc.contributor.authorMajid, Walid A.
dc.contributor.authorBlumer, Harsha
dc.contributor.authorHessels, Jason W.T.
dc.contributor.authorGawroński, Marcin P.
dc.contributor.authorBezrukovs, Vladislavs
dc.contributor.authorOrbidans, Arturs
dc.date.accessioned2022-03-24T13:31:36Z
dc.date.available2022-03-24T13:31:36Z
dc.date.issued2022
dc.description.abstractWe report on NICER X-ray monitoring of the magnetar SGR 1830−0645 covering 223 days following its 2020 October outburst, as well as Chandra and radio observations. We present the most accurate spin ephemerides of the source so far: ν = 0.096008680(2) Hz, Hz s−1, and significant second and third frequency derivative terms indicative of nonnegligible timing noise. The phase-averaged 0.8–7 keV spectrum is well fit with a double-blackbody (BB) model throughout the campaign. The BB temperatures remain constant at 0.46 and 1.2 keV. The areas and flux of each component decreased by a factor of 6, initially through a steep decay trend lasting about 46 days, followed by a shallow long-term one. The pulse shape in the same energy range is initially complex, exhibiting three distinct peaks, yet with clear continuous evolution throughout the outburst toward a simpler, single-pulse shape. The rms pulsed fraction is high and increases from about 40% to 50%. We find no dependence of pulse shape or fraction on energy. These results suggest that multiple hot spots, possibly possessing temperature gradients, emerged at outburst onset and shrank as the outburst decayed. We detect 84 faint bursts with NICER, having a strong preference for occurring close to the surface emission pulse maximum—the first time this phenomenon is detected in such a large burst sample. This likely implies a very low altitude for the burst emission region and a triggering mechanism connected to the surface active zone. Finally, our radio observations at several epochs and multiple frequencies reveal no evidence of pulsed or burst-like radio emission.
dc.identifier.citationYounes, George, Hu, Chin-Ping, Bansal, Karishma, et al.. "X-Ray Burst and Persistent Emission Properties of the Magnetar SGR 1830-0645 in Outburst." <i>The Astrophysical Journal,</i> 924, (2022) IOP Publishing: https://doi.org/10.3847/1538-4357/ac3756.
dc.identifier.digitalYounes_2022
dc.identifier.doihttps://doi.org/10.3847/1538-4357/ac3756
dc.identifier.urihttps://hdl.handle.net/1911/112036
dc.language.isoeng
dc.publisherIOP Publishing
dc.rightsOriginal content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/
dc.titleX-Ray Burst and Persistent Emission Properties of the Magnetar SGR 1830-0645 in Outburst
dc.typeJournal article
dc.type.dcmiText
dc.type.publicationpublisher version
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