A Comprehensive Study of the X‐Ray Bursts from the Magnetar Candidate 1E 2259+586

Gavriil, F. P.; Kaspi, V. M.; Woods, Peter

doi:10.1086/383564

Cited by 121 publications

(196 citation statements)

References 49 publications

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“…The burst intensities follow a power law distribution (Gögüş et al 1999). Similar bursting activity is observed also in AXPs (Gavriil et al 2002;Kaspi et al 2003;Gavriil et al 2004Gavriil et al , 2008Woods et al 2005;Israel et al 2007). However, the AXP bursts detected up to now have much lower (by several orders of magnitude) luminosities.…”

Section: Introductionsupporting

confidence: 64%

“…The value of the hardness of the brightest bursts is affected by the saturation effects in ISGRI and possibly also in the ACS detectors, but for the moderate flux values the observed flux-hardness correlation is robust. The dependence of the hardness of the spectrum on the luminosity was noticed in the bursts of 1E 2259+586 by (Gavriil et al 2004). This type of dependence is the opposite of those observed in SGR bursts, for which a softening of the spectrum with increasing luminosity was observed (Gögüş et al 2001).…”

Section: Statistical Study Of the Burst Propertiesmentioning

confidence: 90%

“…However, the AXP bursts detected up to now have much lower (by several orders of magnitude) luminosities. Besides, contrary to the SGR bursts, which exhibit spectral softening with increasing luminosity (Gögüş et al 2001), the brighter AXP bursts appear to have harder spectra (Gavriil et al 2004). …”

Section: Introductionmentioning

confidence: 94%

“…Major episodes of activity consisting of clusters of ∼10−10 2 bursts are typical for SGRs, but in the case of AXPs such activity was detected only once, in the source 1E 2259+586 in 2003 (Gavriil et al 2004). Below we compare the characteristics of the bursting activity of 1E 1547.0-5408 with those of 1E 2259+586 and of SGRs.…”

Section: Introductionmentioning

confidence: 99%

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SGR-like flaring activity of the anomalous X-ray pulsar 1E 1547.0-5408

Savchenko¹,

Neronov²,

Beckmann³

et al. 2010

A&A

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Aims. We studied an exceptional period of activity of the anomalous X-ray pulsar 1E 1547.0-5408 in January 2009, during which about 200 hard X-ray / soft γ-ray bursts were detected by different instruments on board of ESA's γ-ray observatory INTEGRAL. Methods. The major activity episode (22 January 2009), which was detected by NASA's γ-ray telescope Swift, happened when the source was outside the field of view of all the INTEGRAL instruments. But we were still able to study the statistical properties as well as spectral and timing characteristics of 84 short (100 ms−10 s) bursts from the source during this activity period detected simultaneously by the anti-coincidence shield of the spectrometer SPI on board of INTEGRAL and by the detector of the imager IBIS/ISGRI. Results. We find that the luminosity of the 22 January 2009 bursts of 1E 1547.0-5408 was ≥10 42 erg s −1 above ∼80 keV. This luminosity is comparable to that of the bursts of soft gamma repeaters (SGR) and is at least two orders of magnitude larger than the luminosity of the previously reported bursts from AXPs. Similarly to the SGR bursts, the brightest bursts of 1E 1547.0-5408 consist of a short spike of ∼100 ms duration with a hard spectrum, followed by a softer extended tail of 1-10 s duration, which occasionally exhibits pulsations with the source spin period of ∼2 s. The "short spike + tail" template is not valid for all the observed bursts. We also observe a certain amount of ∼1 s duration bursts either without a spike or with a spike delayed with respect to the onset of the burst. A third type of bursts is the "flat-top" burst of sub-second duration, which is similar to the "precursors" observed in the SGR flares. We find that the bursts of 1E 1547.0-5408 harden with increasing luminosity. Such a behavior is opposite of those observed in SGR bursts, but is similar to the hardness-luminosity relation observed in AXP 1E 2259+586. We confirm the existence of a correlation between the burst fluences and durations and the absence of a correlation between the burst fluence and the waiting time between subsequent bursts, previously established for the AXP 1E 2259+586. Conclusions. The observation of AXP bursts with luminosities comparable to the one of SGR bursts strengthens the conjecture that AXPs and SGRs are different representatives of one and the same source type, and that the AXP and SGR bursts are triggered by a similar type of instabilities.

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Section: Introductionsupporting

confidence: 64%

Section: Statistical Study Of the Burst Propertiesmentioning

confidence: 90%

Section: Introductionmentioning

confidence: 94%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

SGR-like flaring activity of the anomalous X-ray pulsar 1E 1547.0-5408

Savchenko¹,

Neronov²,

Beckmann³

et al. 2010

A&A

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“…The importance of ITDs cannot be overstated, as is the case for other different astrophysical sources, such as the Sun (e.g., Wheatland 2000;Aschwanden & McTiernan 2010), and outbursting magnetars (Göǧüş et al 1999(Göǧüş et al , 2000Gavriil et al 2004). In the case of GRBs a number of papers have investigated this property (McBreen et al 1994;Norris et al 1996).…”

Section: Introductionmentioning

confidence: 99%

Gamma-ray burst engines may have no memory

Baldeschi

Guidorzi

2014

A&A

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Context. A sizeable fraction of gamma-ray burst (GRB) time profiles consist of a temporal sequence of pulses. The nature of this stochastic process carries information on how GRB inner engines work. The so-called interpulse time defines the interval between adjacent pulses, excluding the long quiescence periods during which the signal drops to the background level. It was found by many authors in the past that interpulse times are lognormally distributed, at variance with the exponential case that is expected for a memoryless process. Aims. We investigated whether the simple hypothesis of a temporally uncorrelated sequence of pulses is really to be rejected, as a lognormal distribution necessarily implies. Methods. We selected and analysed a number of multi-peaked CGRO/BATSE GRBs and simulated similar time profiles, with the crucial difference that we assumed exponentially distributed interpulse times, as is expected for a memoryless stationary Poisson process. We then identified peaks in both data sets using a novel peak search algorithm, which is more efficient than others used in the past. Results. We independently confirmed that the observed interpulse time distribution is approximately lognormal. However, we found the same results on the simulated profiles, in spite of the intrinsic exponential distribution. Although intrinsic lognormality cannot be ruled out, this shows that intrinsic interpulse time distribution in real data could still be exponential, while the observed lognormal could be ascribed to the low efficiency of peak search algorithms at short values combined with the limitations of a bin-integrated profile. Conclusions. Our result suggests that GRB engines may emit pulses after the fashion of nuclear radioactive decay, that is, as a memoryless process.

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A classification scheme for magnetars

Göǧüş

2014

Astron Nachr

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We investigate cumulative burst occurrence trends of five soft gamma repeaters (SGRs) and introduce an indicative measure for the duration of their outburst phases. We find a clear distinction between the durations of the active episodes of persistent and transient magnetars: The outburst episodes of the persistent sources are significantly longer ( > ∼ 100 days) than those of transient sources ( < ∼ 10 days). We also investigate burst-induced changes in the radiative behavior of transient sources and suggest a mechanism for the constant flux trend seen in the early phases of the outburst of SGRs with low burst rates.

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A Comprehensive Study of the X‐Ray Bursts from the Magnetar Candidate 1E 2259+586

Cited by 121 publications

References 49 publications

SGR-like flaring activity of the anomalous X-ray pulsar 1E 1547.0-5408

SGR-like flaring activity of the anomalous X-ray pulsar 1E 1547.0-5408

Gamma-ray burst engines may have no memory

A classification scheme for magnetars

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