A New Low Magnetic Field Magnetar: The 2011 Outburst of Swift J1822.3–1606

Rea, N.; Israel, G. L.; Esposito, P.; Pons, José A.; Camero-Arranz, A.; Mignani, Roberto; Turolla, R.; Zane, S.; Burgay, M.; Possenti, A.; Campana, S.; Enoto, T.; Gehrels, N.; Göǧüş, E.; Götz, D.; Kouveliotou, C.; Makishima, Kazuo; Mereghetti, S.; Oates, S. R.; Palmer, D. M.; Perna, Rosalba; Stella, L.; Tiengo, A.

doi:10.1088/0004-637x/754/1/27

Cited by 141 publications

(188 citation statements)

References 59 publications

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“…Subsequently, the source was followed by virtually all the current generation of Xray satellites. The results of the first 9 months of X-ray monitoring of this new magnetar were presented and discussed by Rea et al (2012;hereafter R12), Scholz et al (2012) and Scholz et al (2014). In this work we perform an unprecedent coherent, pulse phase resolved spectroscopy (PPS) analysis spanning more than 400 days of outburst decay (see Fig.…”

Section: Swift J18223-1606mentioning

confidence: 99%

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The outburst decay of the low magnetic field magnetar SWIFT J1822.3−1606: phase-resolved analysis and evidence for a variable cyclotron feature

Castillo

Israel

Tiengo

et al. 2016

Mon. Not. R. Astron. Soc.

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Section: Swift J18223-1606mentioning

confidence: 99%

“…Two more low-field magnetars were recently discovered thanks to their outburst activity, 3XMM J185246.6+003317 (Zhou et al 2014, Rea et al 2014) and SWIFT J1822.3-1606 (Rea et al 2012;Scholtz et al 2012). The latter source was studied through the long-term monitoring that we present in this work.…”

Section: Introductionmentioning

confidence: 99%

The outburst decay of the low magnetic field magnetar SWIFT J1822.3−1606: phase-resolved analysis and evidence for a variable cyclotron feature

Castillo

Israel

Tiengo

et al. 2016

Mon. Not. R. Astron. Soc.

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“…2 for this specific value of the temperature. XMM-Newton satellites found that SGR 1822-1606 rotates with a period of P = 8.44 s and slows down at a rateṖ = 9.1 × 10 −14 (see Rea et al 2012, for details). The corresponding rotation angular velocity of the source is Ω = 2π/P = 0.74 rad s −1 .…”

Section: Prediction Of the Spindown Ratementioning

confidence: 99%

“…(10), which are to be considered to be predictions of the white dwarf model because they were presented in advance of the observational results given in (Rea et al 2013). The situation has become even more striking considering the X-ray timing monitoring with Swift, RXTE, Suzaku, and XMM-Newton satellites of the recently discovered SGR Swift J1822.3-1606 (Rea et al 2012). The rotation period P = 8.437 s and the spindown rateṖ = 9.1×10 −14 were obtained.…”

Section: Introductionmentioning

confidence: 99%

SGR 0418+5729,SwiftJ1822.3-1606, and 1E 2259+586 as massive, fast-rotating, highly magnetized white dwarfs

Boshkayev

Izzo

Rueda

et al. 2013

A&A

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Aims. We describe the so-called low magnetic field magnetars, SGR 0418+5729, Swift J1822.3-1606, and the AXP prototype 1E 2259+586 as massive, fast-rotating, highly magnetized white dwarfs. Methods. We give bounds for the mass, radius, moment of inertia, and magnetic field for these sources by requesting the stability of realistic, general relativistic, uniformly rotating white dwarfs. We also present the theoretical expectation of the infrared, optical, and ultraviolet emission of these objects and show their consistency with the current available observational data. Results. We improve the theoretical prediction of the lower limit of the spindown rate of SGR 0418+5729; for a white dwarf close to its maximum stable mass we obtain the very stringent interval for the spindown rate of 4.1 × 10 −16 <Ṗ < 6 × 10 −15 , where the upper value is the known observational limit. A lower limit has been also set for Swift J1822.3-1606, whose spindown rate is not yet fully confirmed. Our model provides for the sourceṖ ≥ 2.13 × 10 −15 if the star is close to its maximum stable mass. We give in addition the frequencies at which absorption features could be present in the spectrum of these sources as the result of the scattering of photons with the quantized electrons by the surface magnetic field.Key words. stars: magnetic field -stars: rotation -white dwarfs -stars: magnetars IntroductionSoft gamma-ray repeaters (SGRs) and anomalous X-ray pulsars (AXPs) are a class of compact objects that show interesting observational properties (see, e.g., Mereghetti 2008): rotational periods in the range P ∼ (2−12) s, spindown ratesṖ ∼ (10 −13 -10 −10 ), strong outburst of energies ∼(10 41 −10 43 ) erg, and in the case of SGRs, giant flares of even large energies ∼(10 44 -10 47 ) erg.The most popular model for the description of SGRs and AXPs, the magnetar model, is based on a neutron star of fiducial parameters M = 1.4 M , R = 10 km, and a moment of inertia I = 10 45 g cm 2 . It needs a neutron star magnetic field larger than the critical field for vacuum polarization B c = m 2 e c 3 /(e ) = 4.4 × 10 13 G in order to explain the observed X-ray luminosity in terms of the release of magnetic energy (Duncan & Thompson 1992; Thompson & Duncan 1995). There exist in the literature other models still based on neutron stars but of ordinary fields B ∼ 10 12 G; these models involve either the generation of drift waves in the magnetosphere or the accretion of fallback material via a circumstellar disk (see Malov 2010;Trümper et al. 2013, respectively, and references therein).Turning to the experimental point of view, the observation of SGR 0418+5729 with a rotational period of P = 9.08 s, an upper limit of the first time derivative of the rotational perioḋ P < 6.0 × 10 −15 (Rea et al. 2010), and an X-ray luminosity of L X = 6.2 × 10 31 erg s −1 can be considered as the Rosetta Stone for alternative models of SGRs and AXPs. The inferred upper limit of the surface magnetic field of SGR 0418+5729, B < 7.5 × 10 12 G; which describes it as a neutr...

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“…Corresponding author: D. Hadasch, hadasch@ieec.uab.es magnetic fields (∼10 14 −10 15 Gauss) that are ∼10−1000 times higher than the average value in radio pulsars, near or even above the quantum electrodynamic field strength, B QED = m 2 e c 3 /e ∼ 4.4 × 10 13 G (Harding & Lai 2006), although with two exceptions (Rea et al 2010(Rea et al , 2012. They have bright X-ray luminosities (L x ∼ 10 32 −10 36 erg s −1 ) from 0.1-300 keV, longer rotation periods than most ordinary radio pulsars (∼2-12 s), and very high period derivatives (∼10 −13 -10 −11 s s −1 ).…”

Section: Introductionmentioning

confidence: 99%

Observations of the magnetars 4U 0142+61 and 1E 2259+586 with the MAGIC telescopes

Aleksić

Antonelli

Antoranz

et al. 2012

A&A

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Context. Magnetars are an extreme, highly magnetized class of isolated neutron stars whose large X-ray luminosity is believed to be driven by their high magnetic field. Aims. We study for the first time the possible very high energy γ-ray emission above 100 GeV from magnetars, observing the sources 4U 0142+61 and 1E 2259+586. Methods. We observed the two sources with atmospheric Cherenkov telescopes in the very high energy range (E > 100 GeV). 4U 0142+61 was observed with the MAGIC I telescope in 2008 for about 25 h and 1E 2259+586 was observed with the MAGIC stereoscopic system in 2010 for about 14 h. The data were analyzed with the standard MAGIC analysis software. Results. Neither magnetar was detected. Upper limits to the differential and integral flux above 200 GeV were computed using the Rolke algorithm. We obtain integral upper limits to the flux of 1.52 × 10 −12 cm −2 s −1 and 2.7 × 10 −12 cm −2 s −1 with a confidence level of 95% for 4U 0142+61 and 1E 2259+586, respectively. The resulting differential upper limits are presented together with X-ray data and upper limits in the GeV energy range.

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A New Low Magnetic Field Magnetar: The 2011 Outburst of Swift J1822.3–1606

Abstract: We report on the long-term X-ray monitoring with Swift, RXTE, Suzaku, Chandra, and

Cited by 141 publications

References 59 publications

The outburst decay of the low magnetic field magnetar SWIFT J1822.3−1606: phase-resolved analysis and evidence for a variable cyclotron feature

The outburst decay of the low magnetic field magnetar SWIFT J1822.3−1606: phase-resolved analysis and evidence for a variable cyclotron feature

SGR 0418+5729,SwiftJ1822.3-1606, and 1E 2259+586 as massive, fast-rotating, highly magnetized white dwarfs

Observations of the magnetars 4U 0142+61 and 1E 2259+586 with the MAGIC telescopes

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