File Download
  Links for fulltext
     (May Require Subscription)
Supplementary

Article: The spin-down of Swift J1822.3-1606: A new galactic magnetar

TitleThe spin-down of Swift J1822.3-1606: A new galactic magnetar
Authors
KeywordsPulsars: Individual (Swift J1822.3-1606)
Stars: Magnetars
Stars: Neutron
X-Rays: Bursts
Issue Date2011
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205
Citation
Astrophysical Journal Letters, 2011, v. 743 n. 2, article no. L38 How to Cite?
AbstractOn 2011 July 14, a new magnetar candidate, Swift J1822.3-1606, was identified via a rate trigger on the Swift/Burst Alert Telescope. Here we present an initial analysis of the X-ray properties of the source, using data from the Rossi X-ray Timing Explorer, Swift, and the Chandra X-ray Observatory, spanning 2011 July 16-October 8. We measure a precise spin period of P = 8.43771968(6)s and a spin-down rate of , at MJD 55761.0, corresponding to an inferred surface dipole magnetic field of B = 4.7(2) × 10 13G, the second lowest thus far measured for a magnetar, though similar to those of 1E 2259+586 and several high-magnetic field radio pulsars. We show that the flux decay in the 1-10keV band is best fit by a double exponential with timescales of 9 1 and 55 9days. The pulsed count rate decay in the 2-10keV band, by contrast, is better fit by a single exponential decay with timescale 15.9 0.2days. After increasing from 35% for 20days after the onset of the outburst, the pulsed fraction in the 2-10keV band remained constant at 45%. We argue that these properties confirm this source to be a new member of the class of objects known as magnetars. We consider the distribution of magnetar periods and inferred dipole magnetic field strengths, showing that the former appears flat in the 2-12s range, while the latter appears peaked in the 10 14-10 15G range. © 2011. The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/180502
ISSN
2015 Impact Factor: 5.487
2015 SCImago Journal Rankings: 3.369
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorLivingstone, MAen_US
dc.contributor.authorScholz, Pen_US
dc.contributor.authorKaspi, VMen_US
dc.contributor.authorNg, CYen_US
dc.contributor.authorGavriil, FPen_US
dc.date.accessioned2013-01-28T01:38:54Z-
dc.date.available2013-01-28T01:38:54Z-
dc.date.issued2011en_US
dc.identifier.citationAstrophysical Journal Letters, 2011, v. 743 n. 2, article no. L38en_US
dc.identifier.issn2041-8205en_US
dc.identifier.urihttp://hdl.handle.net/10722/180502-
dc.description.abstractOn 2011 July 14, a new magnetar candidate, Swift J1822.3-1606, was identified via a rate trigger on the Swift/Burst Alert Telescope. Here we present an initial analysis of the X-ray properties of the source, using data from the Rossi X-ray Timing Explorer, Swift, and the Chandra X-ray Observatory, spanning 2011 July 16-October 8. We measure a precise spin period of P = 8.43771968(6)s and a spin-down rate of , at MJD 55761.0, corresponding to an inferred surface dipole magnetic field of B = 4.7(2) × 10 13G, the second lowest thus far measured for a magnetar, though similar to those of 1E 2259+586 and several high-magnetic field radio pulsars. We show that the flux decay in the 1-10keV band is best fit by a double exponential with timescales of 9 1 and 55 9days. The pulsed count rate decay in the 2-10keV band, by contrast, is better fit by a single exponential decay with timescale 15.9 0.2days. After increasing from 35% for 20days after the onset of the outburst, the pulsed fraction in the 2-10keV band remained constant at 45%. We argue that these properties confirm this source to be a new member of the class of objects known as magnetars. We consider the distribution of magnetar periods and inferred dipole magnetic field strengths, showing that the former appears flat in the 2-12s range, while the latter appears peaked in the 10 14-10 15G range. © 2011. The American Astronomical Society. All rights reserved.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/2041-8205en_US
dc.relation.ispartofAstrophysical Journal Lettersen_US
dc.subjectPulsars: Individual (Swift J1822.3-1606)en_US
dc.subjectStars: Magnetarsen_US
dc.subjectStars: Neutronen_US
dc.subjectX-Rays: Burstsen_US
dc.titleThe spin-down of Swift J1822.3-1606: A new galactic magnetaren_US
dc.typeArticleen_US
dc.identifier.emailNg, CY: stephen_ng@hku.hken_US
dc.identifier.authorityNg, CY=rp01706en_US
dc.description.naturelink_to_OA_fulltexten_US
dc.identifier.doi10.1088/2041-8205/743/2/L38en_US
dc.identifier.scopuseid_2-s2.0-83055188848en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-83055188848&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume743en_US
dc.identifier.issue2en_US
dc.identifier.isiWOS:000298152500013-
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridLivingstone, MA=9434675600en_US
dc.identifier.scopusauthoridScholz, P=44561412500en_US
dc.identifier.scopusauthoridKaspi, VM=7006755510en_US
dc.identifier.scopusauthoridNg, CY=24830903500en_US
dc.identifier.scopusauthoridGavriil, FP=6602456240en_US
dc.customcontrol.immutablejt 130808-

Export via OAI-PMH Interface in XML Formats


OR


Export to Other Non-XML Formats