A Major Soft Gamma Repeater-like Outburst and Rotation Glitch in the No-longer-so-anomalous X-Ray Pulsar 1E 2259+586

Kaspi, V. M.; Gavriil, F. P.; Woods, P. M.; Jensen, Joseph B.; Roberts, M. S. E.; Chakrabarty, Deepto

doi:10.1086/375683

Cited by 246 publications

(154 citation statements)

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“…than the ones of SGR 0418+5729 and SGR 1822-1606, indicating that 1E 2259+586 is a very active source in which glitches and outburst activity, such as those observed in 2002 (Kaspi et al 2003;Woods et al 2004), can occur with relatively high frequency. It is interesting to note that glitches of minor intensity |ΔP|/P 10 −7 can be even more frequent, with recurrence times of 4 yr.…”

Section: Solidification and Glitchesmentioning

confidence: 92%

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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Section: Solidification and Glitchesmentioning

confidence: 92%

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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“…The detection of a ∼8 s periodicity in the decaying tail of a very intense (∼10 44 erg) and long (several minutes) event, known as giant flare, from SGR 0526-66 on 1979 March 5th (Mazets et al 1979) suggested the association of SGRs with neutron stars. A small sample of peculiar X-ray pulsars, namely the Anomalous X-ray Pulsars (AXPs) has been proposed to be closely related to SGRs based on similar properties, namely their period P (in the 5-12 s range), their period derivativeṖ (10 −10 -10 −13 s s −1 range), and X-ray bursts (Kouveliotou et al 1998;Kaspi et al 2003;Gavriil et al 2002).…”

Section: Introductionmentioning

confidence: 99%

Discovery and monitoring of the likely IR counterpart of SGR 1806–20 during the 2004 γ-ray burst-active state

Israel¹,

Covino

Mignani

et al. 2005

A&A

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Abstract. The sky region including the Chandra position of SGR 1806-20 was monitored in the IR band during 2004, following its increased high energy bursting activity. Observations were performed using NAOS-CONICA, the adaptive optics IR camera mounted on Yepun VLT, which provided images of unprecedented quality (FWHM better than 0. 1). After the 2004 December 27th giant flare, the source position has been nailed by VLA observations of its radio counterpart, reducing the positional uncertainty to 0. 04. Using IR data from our monitoring campaign, we discovered the likely IR counterpart to SGR 1806-20 based on positional coincidence with the Chandra and VLA uncertainty regions and flux variability of a factor of about 2 correlated with that at higher energies. We compare our findings with other isolated neutron star classes thought to be related, at some level, with SGRs.

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“…1E 2259+586 has been monitored with Rossi X-ray Timing Explorer and Swift X-ray Telescope over almost the last two decades, showing a stable spin-down rate, with the exception of two spin-up glitches in 2002 [10] and 2007 [11], a timing event in 2009 [11], and this anti-glitch in 2012.…”

mentioning

confidence: 99%

A simple mechanism for the anti-glitch observed in AXP 1E 2259+586

García¹,

Ranea‐Sandoval²

2015

Monthly Notices of the Royal Astronomical Society: Letters

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In this short communication we present a simple internal mechanism that accounts for the recently observed anti-glitch in magnetar 1E 2259+586.We propose that the decay of an internal toroidal magnetic field component would de-stabilize an originally stable prolate star configuration. Then, the subsequent rearrangement of the stellar structure would give rise to a "more spherical" configuration, resulting in a sudden spin-down of the whole star.We present here some order of magnitude calculation to give confidence to this scenario, using the simplest analytical stellar model and let more detailed calculations for a more technical future paper.

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A Major Soft Gamma Repeater-like Outburst and Rotation Glitch in the No-longer-so-anomalous X-Ray Pulsar 1E 2259+586

Cited by 246 publications

References 25 publications

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

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

Discovery and monitoring of the likely IR counterpart of SGR 1806–20 during the 2004 γ-ray burst-active state

A simple mechanism for the anti-glitch observed in AXP 1E 2259+586

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