<i>CHANDRA</i>AND<i>RXTE</i>OBSERVATIONS OF 1E 1547.0–5408: COMPARING THE 2008 AND 2009 OUTBURSTS

Ng, C.‐Y.; Kaspi, V. M.; Dib, Rim; Olausen, S. A.; Scholz, Paul; Güver, T.; Özel, Feryal; Gavriil, F. P.; Woods, P. M.

doi:10.1088/0004-637x/729/2/131

Cited by 45 publications

(71 citation statements)

References 42 publications

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“…Here and thereafter 1σ c.l uncertainty is reported, unless otherwise specified. These values are consistent with those reported by Kaneko et al (2010) and Ng et al (2011) based on Fermi and RXT E data only, respectively. Time residuals with respect to the timing solution are plotted in Fig.…”

Section: Timing Analysissupporting

confidence: 92%

“…By includingP component in the fit, we derived a 3σ upper limit of 1.8 × 10 −17 s/s 2 (absolute value). This is smaller then theP component detected during the 2008 outburst Ng et al 2011). The timing solution obtained during 2008 outburst consequently resulted to be more complex then the 2009 timing solution.…”

Section: Timing Analysismentioning

confidence: 78%

“…However, taking into account a longer baseline for the January 2009 outburst, using the Swift data covering the time period between January 2009 and June 2010, the PF showed the same evolution in time as in the case of the October 2008 outburst. Indeed in both cases, after the outburst onset, there was an anti-correlation between the X-ray flux and the PF; higher flux levels were associated to lower PFs (see also Ng et al 2011). After the October 2008 outburst the PF increased from ∼20% up to ∼50% while after the January 2009 outburst the PF increased from 8 ± 2% to 33 ± 5%.…”

Section: Pulsed Fractionmentioning

confidence: 83%

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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: Timing Analysissupporting

confidence: 92%

Section: Timing Analysismentioning

confidence: 78%

Section: Pulsed Fractionmentioning

confidence: 83%

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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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“…However, following the first day, the pulsed fraction was still significantly lower than the preburst pulsed fraction. This anti-correlation between pulsed fraction and flux is presented with the addition of Chandra and XMM-Newton data in Ng et al (2011), who suggest it could be due to an increase in the emitting area of a thermal hot spot, which would cause the emission to be observable during a greater portion of the phase of the pulsar. We note that both correlations (Gotthelf et al 2004;Zhu et al 2008) and anti-correlations (Israel et al 2007;Tam et al 2008) between pulsed fraction and flux have been observed in magnetar outbursts.…”

Section: Persistent Fluxmentioning

confidence: 83%

The 2009 Outburst of Magnetar 1e 1547--5408: Persistent Radiative and Burst Properties

Scholz¹,

Kaspi²

2011

ApJ

Self Cite

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The magnetar 1E 1547−5408 recently exhibited two periods of outburst, beginning on 2008 October 3 and 2009 January 22. Here we present an analysis of the persistent radiative evolution and a statistical study of the burst properties during the 2009 outburst using the Swift X-ray Telescope (XRT). We find that the 1-10 keV flux increased by a factor of ∼ 500 and hardened significantly, peaking ∼ 6 hours after the onset of the outburst. The observed pulsed fraction exhibited an anticorrelation with phase-averaged flux. Properties of the several hundred X-ray bursts during the 2009 outburst were determined and compared to those from other magnetar outburst events. We find that the peaks of the bursts occur randomly in phase but that the folded counts that compose the bursts exhibit a pulse which is misaligned with the persistent pulse phase. We also report a correlation between burst hardness and flux. We compare the hardness-flux evolution of the persistent emission of both outbursts to those from other magnetars and find that although there does exist an overall trend, the degree of hardening for a given increase in flux is not uniform from source to source. These results are discussed in the context of previous results and within the magnetar model.

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“…Therefore, in the case of AXPs and SGRs, the spectra provide a handle on the magnetic field strength on the neutron star surface. The magnetic field strengths of numerous sources have been measured by modeling their spectra with strongly magnetic neutron star atmosphere models (Güver et al 2007Özel et al 2008;Gögüş et al 2011;Ng et al 2011;Güver et al 2011). The dipole magnetic field strength B d inferred from their measured rate of spindown using Equation 7 is plotted against the spectroscopic magnetic field strengths B s obtained for these sources in Figure 13.…”

Section: Neutron Star Magnetic Field Geometry and Evolutionmentioning

confidence: 99%

Surface emission from neutron stars and implications for the physics of their interiors

Özel

2012

Rep. Prog. Phys.

124

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Abstract. Neutron stars are associated with diverse physical phenomena that take place in conditions characterized by ultrahigh densities as well as intense gravitational, magnetic, and radiation fields. Understanding the properties and interactions of matter in these regimes remains one of the challenges in compact object astrophysics. Photons emitted from the surfaces of neutron stars provide direct probes of their structure, composition, and magnetic fields. In this review, I discuss in detail the physics that governs the properties of emission from the surfaces of neutron stars and their various observational manifestations. I present the constraints on neutron star radii, core and crust composition, and magnetic field strength and topology obtained from studies of their broadband spectra, evolution of thermal luminosity, and the profiles of pulsations that originate on their surfaces.

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CHANDRAANDRXTEOBSERVATIONS OF 1E 1547.0–5408: COMPARING THE 2008 AND 2009 OUTBURSTS

Cited by 45 publications

References 42 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

The 2009 Outburst of Magnetar 1e 1547--5408: Persistent Radiative and Burst Properties

Surface emission from neutron stars and implications for the physics of their interiors

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