Swift Observations of Two Outbursts From the Magnetar 4u 0142+61

Archibald, R. F.; Kaspi, V. M.; Scholz, Paul; Beardmore, A. P.; Gehrels, N.; Kennea, J. A.

doi:10.3847/1538-4357/834/2/163

Cited by 23 publications

(28 citation statements)

References 53 publications

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“…Largest spin-down glitches observed are, the glitch of 1E 2259+586 with ∆ν/ν ∼ 10 −6 (Archibald et al 2013) and the glitch of SGR 1900+14 with ∆ν/ν ∼ 10 −4 within 80 days after a large outburst (Woods et al 1999; Thompson et al 2000). There are a few net spin-down glitches (İçdem et al 2012;Saşmaz Muş & Gögüş 2013;Archibald et al 2017) together with a large number of spin-up glitches (Dib & Kaspi 2014). Large spin-down glitches can be explained by particle outflow from magnetic multipoles during an outburst, while this process induces vortex inflow from the crust.…”

Section: The Glitchmentioning

confidence: 95%

Discovery of a glitch in the accretion-powered pulsar SXP 1062

Serim

Şahiner

Cerri-Serim

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present timing analysis of the accretion powered pulsar SXP 1062, based on the observations of Swift, XMM-Newton and Chandra satellites covering a time span of about 2 years. We obtain a phase coherent timing solution which shows that SXP 1062 has been steadily spinning down with a rate − 4.29(7) × 10 −14 Hz s −1 leading to a surface magnetic field estimate of about 1.5 × 10 14 G. We also resolve the binary orbital motion of the system from X-ray data which confirms an orbital period of 656(2) days. On MJD 56834.5, a sudden change in pulse frequency occurs with ∆ν = 1.28(5) × 10 −6 Hz, which indicates a glitch event. The fractional size of the glitch is ∆ν/ν ∼ 1.37(6) ×10 −3 and SXP 1062 continues to spin-down with a steady rate after the glitch. A short X-ray outburst 25 days prior to the glitch does not alter the spin-down of the source; therefore the glitch should be associated with the internal structure of the neutron star. While glitch events are common for isolated pulsars, the glitch of SXP 1062 is the first confirmation of the observability of this type of events among accretion powered pulsars. Furthermore, the value of the fractional change of pulse frequency ensures that we discover the largest glitch reported up to now.

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Section: The Glitchmentioning

confidence: 95%

Discovery of a glitch in the accretion-powered pulsar SXP 1062

Serim

Şahiner

Cerri-Serim

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…1E 1048.1−5937 was monitored regularly with the Swift-XRT since 2011 July as part of a campaign to study several magnetars (see e.g. Scholz et al 2014;Archibald et al 2015Archibald et al , 2017. The XRT was operated in Windowed-Timing (WT) mode for all observations, having a time resolution of 1.76 ms, and only one dimension of spatial resolution.…”

Section: Swift Xrt Monitoringmentioning

confidence: 99%

“…Data were downloaded from the HEASARC Swift archive, reduced using the xrtpipeline standard reduction script, and time-corrected to the Solar System Barycenter using HEASOFT v6.22. Following this, we processed the data in the same manner described by Archibald et al (2017).…”

Section: Swift Xrt Monitoringmentioning

confidence: 99%

Two New Outbursts and Transient Hard X-Rays from 1E 1048.1-5937

Archibald

Scholz

Kaspi

et al. 2020

ApJ

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Since its discovery, 1E 1048.1−5937 has been one of the most active magnetars, both in terms of radiative outbursts, and changes to its spin properties. Here we report on a continuing monitoring campaign with the Neil Gehrels Swift Observatory X-ray Telescope in which we observe two new outbursts from this source. The first outburst occurred in 2016 July, and the second in 2017 December, reaching peak 0.5-10 keV absorbed fluxes of 3.2 +0.2 −0.3 × 10 −11 erg s −1 cm −2 and 2.2 +0.2 −0.2 × 10 −11 erg s −1 cm −2 , respectively, factors of ∼5 and ∼ 4 above the quiescent flux. Both new outbursts were accompanied by spin-up glitches with amplitudes of ∆ν = 4.47(6) × 10 −7 Hz and ∆ν = 4.32(5) × 10 −7 Hz, respectively. Following the 2016 July outburst, we observe, as for past outbursts, a period of delayed torque fluctuations, which reach a peak spin-down of 1.73 ± 0.01 times the quiescent rate, and which dominates the spin evolution compared to the spin-up glitches. We also report an observation near the peak of the first of these outbursts with NuSTAR in which hard X-ray emission is detected from the source. This emission is well characterized by an absorbed blackbody plus a broken power law, with a powerlaw index above 13.4 ± 0.6 keV of 0.5 +0.3 −0.2 , similar to those observed in both persistent and transient magnetars. The hard X-ray results are broadly consistent with models of electron/positron cooling in twisted magnetic field bundles in the outer magnetosphere. However the repeated outbursts and associated torque fluctuations in this source remain puzzling.

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“…We select the magnetar sample from the McGill Online Magnetar Catalog (http://www.physics.mcgill.ca/pulsar/magnetar/main.html), which categorizes 23 confirmed magnetars (Olausen & Kaspi ). The glitch sample from five bright magnetars is adopted from Dib & Kaspi () with a few updates (Archibald et al , ). For other magnetars, we obtain glitches in CXOU J164710.2–455216, 1E 1547.0–5408, SGR J1745–2900, and Swift J1822.3–1606.…”

Section: Glitch Samplementioning

confidence: 99%

“…We do not include them in the following analysis because their mechanism could be dramatically different from canonical glitches (Archibald et al ; Dib & Kaspi ; Pintore et al ). Some antiglitches are likely over‐recovery from spin‐up glitches and we include their spin‐up measurement in the analysis (Archibald et al ; Gavriil et al ). All the sampled glitches are listed in Table .…”

Section: Glitch Samplementioning

confidence: 99%

On the connection between radiative outbursts and timing irregularities in magnetars

2019

Astron Nachr

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Magnetars are strongly magnetized pulsars and they occasionally show violent radiative outbursts. They also often exhibit glitches that are sudden changes in the spin frequency. It was found that some glitches were associated with outbursts but their connection remains unclear. We present a systematic study to identify possible correlations between them. We find that the glitch size of magnetars likely shows a bimodal distribution, different from the distribution of the Vela-like recurrent glitches but consistent with the high-end of that of normal pulsars. A glitch is likely a necessary condition for an outburst but not a sufficient condition because only 30% of glitches were associated with outbursts. In the outburst cases, the glitches tend to induce larger frequency changes compared to those unassociated ones. We argue that a larger glitch is more likely to trigger the outburst mechanism, either by reconfiguration of the magnetosphere or deformation of the crust. A more frequent and deeper monitoring of magnetars is necessary for further investigation of their connection.

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Swift Observations of Two Outbursts From the Magnetar 4u 0142+61

Cited by 23 publications

References 53 publications

Discovery of a glitch in the accretion-powered pulsar SXP 1062

Discovery of a glitch in the accretion-powered pulsar SXP 1062

Two New Outbursts and Transient Hard X-Rays from 1E 1048.1-5937

On the connection between radiative outbursts and timing irregularities in magnetars

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