A new low magnetic field magnetar: the 2011 outburst of Swift J1822.3–1606

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Title: A new low magnetic field magnetar: the 2011 outburst of Swift J1822.3–1606
Authors: Rea, Nanda | Israel, Gian Luca | Esposito, Paolo | Pons, José A. | Camero-Arranz, Ascensión | Mignani, Roberto P. | Turolla, Roberto | Zane, Silvia | Burgay, Marta | Possenti, Andrea | Campana, Sergio | Enoto, Teru | Gehrels, Neil | Göğüş, Ersin | Götz, Diego | Kouveliotou, Chryssa | Makishima, Kazuo | Mereghetti, Sandro | Oates, Sam R. | Palmer, David M. | Perna, Rosalba | Stella, Luigi | Tiengo, Andrea
Research Group/s: Astrofísica Relativista
Center, Department or Service: Universidad de Alicante. Departamento de Física Aplicada
Keywords: Stars: individual (Swift J1822.3–1606) | Stars: magnetars | Stars: neutron | X-rays: bursts | X-rays: stars
Knowledge Area: Astronomía y Astrofísica
Issue Date: 2-Jul-2012
Publisher: IOP Publishing
Citation: The Astrophysical Journal. 2012, 754(1): 27. doi:10.1088/0004-637X/754/1/27
Abstract: We report on the long-term X-ray monitoring with Swift, RXTE, Suzaku, Chandra, and XMM-Newton of the outburst of the newly discovered magnetar Swift J1822.3–1606 (SGR 1822–1606), from the first observations soon after the detection of the short X-ray bursts which led to its discovery, through the first stages of its outburst decay (covering the time span from 2011 July until the end of 2012 April). We also report on archival ROSAT observations which detected the source during its likely quiescent state, and on upper limits on Swift J1822.3–1606's radio-pulsed and optical emission during outburst, with the Green Bank Telescope and the Gran Telescopio Canarias, respectively. Our X-ray timing analysis finds the source rotating with a period of P = 8.43772016(2) s and a period derivative P = 8.3(2)×10−14 s s−1, which implies an inferred dipolar surface magnetic field of B sime 2.7 × 1013 G at the equator. This measurement makes Swift J1822.3–1606 the second lowest magnetic field magnetar (after SGR 0418+5729). Following the flux and spectral evolution from the beginning of the outburst, we find that the flux decreased by about an order of magnitude, with a subtle softening of the spectrum, both typical of the outburst decay of magnetars. By modeling the secular thermal evolution of Swift J1822.3–1606, we find that the observed timing properties of the source, as well as its quiescent X-ray luminosity, can be reproduced if it was born with a poloidal and crustal toroidal fields of Bp ~ 1.5 × 1014 G and B tor ~ 7 × 1014 G, respectively, and if its current age is ~550 kyr.
Sponsor: N.R. is supported by a Ramon y Cajal Research Fellowship, and by grants AYA2009-07391, SGR2009-811, TW2010005, and iLINK 2011-0303. The Italian authors are supported by Agenzia Spaziale Italiana (ASI), Ministero dell’Istruzione, Università e Ricerca Scientifica e Tecnologica (MIUR–COFIN), and Istituto Nazionale di Astrofisica (PRIN-INAF) grants. P.E. acknowledges financial support from the Autonomous Region of Sardinia through a research grant under the program PO Sardegna FSE 2007–2013, L.R. 7/2007 “Promoting scientific research and innovation technology in Sardinia.” C.K. was partially supported by NASA grant NNH07ZDA001-GLAST.
URI: http://hdl.handle.net/10045/33857
ISSN: 0004-637X (Print) | 1538-4357 (Online)
DOI: 10.1088/0004-637X/754/1/27
Language: eng
Type: info:eu-repo/semantics/article
Rights: © 2012. The American Astronomical Society
Peer Review: si
Publisher version: http://dx.doi.org/10.1088/0004-637X/754/1/27
Appears in Collections:INV - Astrofísica Relativista - Artículos de Revistas

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