Correlated Infrared and X-Ray Flux Changes Following the 2002 June Outburst of the Anomalous X-Ray Pulsar 1E 2259+586

Tam, Cindy R.; Kaspi, V. M.; Kerkwijk, M. H. van; Durant, Martin

doi:10.1086/426963

Cited by 59 publications

(78 citation statements)

References 28 publications

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“…For example, a correlation in the decays of the X-ray and near-IR fluxes in 1E 2259+586 was observed following the 2002 outburst (Tam et al 2004); a similar correlation was reported for XTE J1810−197 . However, in other instances, the two fluxes were not correlated, as for 1E 1048−5937 , and Durant, van Kerkwijk, & Hulleman 2004.…”

Section: Other Wavelengthssupporting

confidence: 65%

10 years of RXTE monitoring of anomalous X-ray pulsar 4U 0142+61: long-term variability

Dib¹,

Kaspi²,

Gavriil³

2007

Isolated Neutron Stars: From the Surface to the Interior

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We report on 10 years of monitoring of the 8.7-s Anomalous X-ray Pulsar 4U 0142+61 using the Rossi X-Ray Timing Explorer (RXTE). This pulsar exhibited stable rotation from 2000 March until 2006 February: the RMS phase residual for a spin-down model which includes ν, ν, and ν is 2.3%. We report a possible phase-coherent timing solution valid over a 10-yr span extending back to March 1996. A glitch may have occured between 1998 and 2000, but is not required by the existing timing data. The pulse profile has been evolving since 2000. In particular, the dip of emission between its two peaks got shallower between 2002 and 2006, as if the profile were evolving back to its pre-2000 morphology, following an earlier event, which possibly also included the glitch suggested by the timing data. These profile variations are seen in the 2−4 keV band but not in 6−8 keV. We also detect a slow increase in the pulsed flux between 2002 May and 2004 December, such that it has risen by 36±3% over 2.6 years in the 2−10 keV band. The pulsed flux variability and the narrow-band pulse profile changes present interesting challenges to aspects of the magnetar model.

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Section: Other Wavelengthssupporting

confidence: 65%

10 years of RXTE monitoring of anomalous X-ray pulsar 4U 0142+61: long-term variability

Dib¹,

Kaspi²,

Gavriil³

2007

Isolated Neutron Stars: From the Surface to the Interior

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show abstract

“…Moreover, it has become evident that X-ray flux enhancement of the persistent emission of SGRs is correlated with their burst rate, making it difficult to compare the fluxes among different SGRs without knowing their burst history (see Woods & Thompson 2004). Tam et al (2004) argued that IR thermal surface emission (within the magnetar model) is ruled out during the correlated X-ray/IR flux decay phases of 1E 2259+586 (implausibly high implied brightness temperature), suggesting the magnetospheric origin for the IR enhancement. Alternatively, the IR flux can be due to reradiation by material in the vicinity of the the pulsar.…”

Section: Discussionmentioning

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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“…The IR and X-ray fluxes subsequently decayed in a similar way, suggesting a close link between the emission processes in these two energy ranges. This was interpreted as evidence for a non-thermal, magnetospheric origin of the IR radiation [230], but Ertan et al [62] showed that the data can also be explained as emission from a residual disk pushed away by an energetic flare and gradually relaxing back to its original configuration.…”

Section: Optical and Infraredmentioning

confidence: 99%

The strongest cosmic magnets: soft gamma-ray repeaters and anomalous X-ray pulsars

Mereghetti

2008

Astron Astrophys Rev

696

766

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Two classes of X-ray pulsars, the Anomalous X-ray Pulsars and the Soft Gamma-ray Repeaters, have been recognized in the last decade as the most promising candidates for being magnetars: isolated neutron stars powered by magnetic energy. I review the observational properties of these objects, focussing on the most recent results, and their interpretation in the magnetar model. Alternative explanations, in particular those based on accretion from residual disks, are also considered. The possible relations between these sources and other classes of neutron stars and astrophysical objects are also discussed.

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Correlated Infrared and X-Ray Flux Changes Following the 2002 June Outburst of the Anomalous X-Ray Pulsar 1E 2259+586

Cited by 59 publications

References 28 publications

10 years of RXTE monitoring of anomalous X-ray pulsar 4U 0142+61: long-term variability

10 years of RXTE monitoring of anomalous X-ray pulsar 4U 0142+61: long-term variability

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

The strongest cosmic magnets: soft gamma-ray repeaters and anomalous X-ray pulsars

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