From outburst to quiescence: the decay of the transient AXP XTE J1810-197

Bernardini, F.; Israel, G. L.; Dall’Osso, S.; Stella, L.; Rea, N.; Zane, S.; Turolla, R.; Perna, Rosalba; Falanga, M.; Campana, S.; Götz, D.; Mereghetti, S.; Tiengo, A.

doi:10.1051/0004-6361/200810779

Cited by 70 publications

(120 citation statements)

References 62 publications

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“…The portion of the emitting region on the NS surface which is in view does not vary significantly as the star rotates, resulting in a low level of modulation. Indeed the radius of the BB responsible for the magnitude of the modulation is rather high, R BB ∼ 3 km, compared for example to that measured during the outburst of another transient magnetar, XTE J1810−197, for which R bb ≤ 1 km (with kT ∼ 0.6 keV) and the PF was > ∼ 50% (Bernardini et al 2009). …”

Section: Pulsed Fractionmentioning

confidence: 79%

“…Ordinarily divided in two classes, there is now increasing evidence that the distinction between AXPs and SGRs originates mainly from the way in which the sources are first discovered (rather than reflect intrinsic physical differences, as also supported by recent MHD simulations, Perna & Pons 2011): AXPs, are detected by their persistent pulsed emission A&A 529, A19 (2011) magnetar from outburst to quiescence so far (Bernardini et al 2009). In the last few years, six other faint X-ray sources underwent similar outbursts (X-ray flux variation of a factor ∼100).…”

Section: Introductionmentioning

confidence: 96%

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Multi-instrument X-ray monitoring of the January 2009 outburst from the recurrent magnetar candidate 1E 1547.0-5408

Bernardini¹,

Israel²,

Stella³

et al. 2011

A&A

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Context. With two consecutive outbursts recorded in four months (October 2008 and January 2009), and a possible third outburst in 2007, 1E 1547.0-5408 is one of the most active transient anomalous X-ray pulsars known so far. Aims. Thanks to extensive X-ray observations, obtained both in the quiescent and active states, 1E 1547.0-5408 represents a very promising laboratory to gain insight into the outburst properties and magnetar emission mechanisms. Methods. We performed a detailed timing and spectral analysis of four Chandra, three INTEGRAL, and one XMM-Newton observations collected over a two week interval after the outburst onset in January 2009. Several Swift pointings, covering a 1.5 year interval, were also analyzed in order to monitor the decay of the X-ray flux. Results. We compare the characteristics of the two outbursts, as well as those of the active and quiescent states. We also discuss the long-term X-ray flux history of 1E 1547.0-5408 since its first detection in 1980, and show that the source displays three flux levels: low, intermediate and high.

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Section: Pulsed Fractionmentioning

confidence: 79%

Section: Introductionmentioning

confidence: 96%

Multi-instrument X-ray monitoring of the January 2009 outburst from the recurrent magnetar candidate 1E 1547.0-5408

Bernardini¹,

Israel²,

Stella³

et al. 2011

A&A

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“…Most recent distance and corresponding peak luminosity estimates for this source are d = 5 kpc, L X = 1.3 × 10 36 erg s −1 (Ibrahim et al 2004), d = 3.3 kpc, L X = 5.8 × 10 35 erg s −1 (Lazaridis et al 2008), and d = 3.5 kpc, L X = 6.6 × 10 35 erg s −1 (Bernardini et al 2009). In our calculations, we take d = 3.5 kpc.…”

Section: Application Of the Model To The X-ray Enhancement Light Curvmentioning

confidence: 85%

“…We pursue the results of the work by Ertan & Erkut (2008) on the X-ray outburst light curve and the spin evolution of the transient AXP XTE J1810-197. The X-ray outburst light curve of this source showed a different decay morphology than those of persistent sources (Ibrahim et al 2004;Bernardini et al 2009). By means of model fits to the X-ray enhancement data, Ertan & Erkut (2008) concluded that this difference could be due to a viscous disk instability (see, e.g., Lasota 2001 for a review of the disk instability model (DIM)) in the fallback disks at a critical temperature in the ∼1000-2000 K range.…”

Section: Introductionmentioning

confidence: 90%

On the X-Ray Outbursts of Transient Anomalous X-Ray Pulsars and Soft Gamma-Ray Repeaters

Çalışkan¹,

Ertan²

2012

ApJ

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We show that the X-ray outburst light curves of four transient anomalous X-ray pulsars (AXPs) and soft gamma-ray repeaters (SGRs), namely, XTE J1810−197, SGR 0501+4516, SGR 1627−41, and CXOU J164710.2−455216, can be produced by the fallback disk model that was also applied to the outburst light curves of persistent AXPs and SGRs in our earlier work. The model solves the diffusion equation for the relaxation of a disk that has been pushed back by a soft gamma-ray burst. The sets of main disk parameters used for these transient sources are very similar to each other and to those employed in our earlier models of persistent AXPs and SGRs. There is a characteristic difference between the X-ray outburst light curves of transient and persistent sources. This can be explained by the differences in the disk surface density profiles of the transient and persistent sources in quiescence indicated by their quiescent X-ray luminosities. Our results imply that a viscous disk instability operating at a critical temperature in the range of ∼1300-2800 K is a common property of all fallback disks around AXPs and SGRs. The effect of the instability is more pronounced and starts earlier for the sources with lower quiescent luminosities, which leads to the observable differences in the X-ray enhancement light curves of transient and persistent sources. A single active disk model with the same basic disk parameters can account for the enhancement phases of both transient and persistent AXPs and SGRs. We also present a detailed parameter study to show the effects of disk parameters on the evolution of the X-ray luminosity of AXPs and SGRs in the X-ray enhancement phases.

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“…This so-called "j-bundle" is the result of a twist of the crust by the starquake that initiated the outburst. As the j-bundle untwists, its boundary recedes toward the magnetic pole; thus, the area of its footpoint decreases, which accounts for the declining blackbody area fitted to the X-ray spectrum (Gotthelf & Halpern 2007;Bernardini et al 2009). …”

Section: Decline Of the X-ray And Radio Luminositymentioning

confidence: 99%

Radio Disappearance of the Magnetar Xte J1810–197 and Continued X-Ray Timing

Camilo

Ransom

Halpern

et al. 2016

ApJ

135

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We report on timing, flux density, and polarimetric observations of the transient magnetar and 5.54 s radio pulsar XTEJ1810−197 using the Green Bank, Nançay, and Parkes radio telescopes beginning in early 2006, until its sudden disappearance as a radio source in late 2008. Repeated observations through 2016 have not detected radio pulsations again. The torque on the neutron star, as inferred from its rotation frequency derivativeṅ, decreased in an unsteady manner by a factor of three in the first year of radio monitoring, until approximately mid-2007. By contrast, during its final year as a detectable radio source, the torque decreased steadily by only 9%. The periodaveraged flux density, after decreasing by a factor of 20 during the first 10 months of radio monitoring, remained relatively steady in the next 22 months, at an average of 0.7±0.3 mJy at 1.4 GHz, while still showing day-to-day fluctuations by factors of a few. There is evidence that during this last phase of radio activity the magnetar had a steep radio spectrum, in contrast to earlier flat-spectrum behavior. No secular decrease presaged its radio demise. During this time, the pulse profile continued to display large variations; polarimetry, including of a new profile component, indicates that the magnetic geometry remained consistent with that of earlier times. We supplement these results with X-ray timing of the pulsar from its outburst in 2003 up to 2014. For the first 4 years, XTEJ1810 −197 experienced non-monotonic excursions in frequency derivative by at least a factor of eight. But since 2007, itsṅ has remained relatively stable near its minimum observed value. The only apparent event in the X-ray record that is possibly contemporaneous with the radio shutdown is a decrease of ≈20% in the hot-spot flux in 2008-2009, to a stable, minimum value. However, the permanence of the high-amplitude, thermal X-ray pulse, even after the (unexplained) radio demise, implies continuing magnetar activity.

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From outburst to quiescence: the decay of the transient AXP XTE J1810-197

Cited by 70 publications

References 62 publications

Multi-instrument X-ray monitoring of the January 2009 outburst from the recurrent magnetar candidate 1E 1547.0-5408

Multi-instrument X-ray monitoring of the January 2009 outburst from the recurrent magnetar candidate 1E 1547.0-5408

On the X-Ray Outbursts of Transient Anomalous X-Ray Pulsars and Soft Gamma-Ray Repeaters

Radio Disappearance of the Magnetar Xte J1810–197 and Continued X-Ray Timing

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