Konus-Wind Observations of the New Soft Gamma-Ray Repeater SGR 0501+4516

Aptekar, R.; Cline, T. L.; Frederiks, D.; Golenetskii, S.; Mazets, E.; Pal'Shin, V.

doi:10.1088/0004-637x/698/2/l82

Cited by 29 publications

(32 citation statements)

References 26 publications

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“…The distance of SGR 0501+4516 is not very well determined, with estimates d = 1.5 kpc (Aptekar et al 2009), d = 4 kpc (Nakagawa et al 2011), d = 5 kpc ), and d = 10 kpc (Enoto et al 2009;Kumar et al 2010). The pre-outburst quiescent (0.1-2.4 keV) flux of this source was reported as ∼4.1 × 10 −12 erg cm −2 s −1 , which corresponds to a 1-10 keV flux of 1.3 × 10 −12 erg cm −2 s −1 .…”

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

confidence: 98%

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

confidence: 98%

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

Çalışkan¹,

Ertan²

2012

ApJ

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“…As discussed above, the main powering mechanisms 6 at work in other kinds of NSs have problems to explain the properties of AXPs/SGRs. This motivated interest in the alternative proposal of a magnetically-powered emission and led to the development of models based on magnetars [36,176,180].…”

Section: Magnetic Energymentioning

confidence: 99%

“…This is enough to power a luminosity of ∼10 35 erg s −1 for ∼10 5 years, a plausible age for AXPs/SGRs, considering their frequent association with supernova remnants (SNRs) or young clusters of massive stars 7 . Slightly higher fields and/or long-lasting episodes with low luminosity (as in transients) make the 6 Another energy source is provided by nuclear reactions. This powers the type I bursts observed in many accreting low mass X-binaries.…”

Section: Magnetic Energymentioning

confidence: 99%

Pulsars and Magnetars

Mereghetti

2013

Braz J Phys

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The high-energy sources known as anomalous X-ray pulsars (AXPs) and soft γ-ray repeaters (SGRs) are well explained as magnetars: isolated neutron stars powered by their own magnetic energy. After explaining why it is generally believed that the traditional energy sources at work in other neutron stars (accretion, rotation, residual heat) cannot power the emission of AXPs/SGRs, I review the observational properties of the twenty AXPs/SGRs currently known and describe the main features of the magnetar model. In the last part of this review I discuss the recent discovery of magnetars with low external dipole field and some of the relations between AXPs/SGRs and other classes of isolated neutron stars.

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“…The SGR J0501+4516 outburst lasted approximately 2 weeks, during which several bright bursts were detected with Swift, GBM, RXTE, Konus-Wind, and Suzaku (Enoto et al 2009;Aptekar et al 2009;Kumar et al 2010, see also Table 1). After the burst activity ceased, the source flux decreased exponentially with an e-folding time of 27.9 ± 2.5 days .…”

Section: Introductionmentioning

confidence: 99%

Fermi/GAMMA-RAY BURST MONITOR OBSERVATIONS OF SGR J0501+4516 BURSTS

Lin

Kouveliotou

Baring

et al. 2011

ApJ

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We present our temporal and spectral analyses of 29 bursts from SGR J0501+4516, detected with the gamma-ray burst monitor on board the Fermi Gamma-ray Space Telescope during 13 days of the source's activation in 2008 (August 22-September 3). We find that the T 90 durations of the bursts can be fit with a log-normal distribution with a mean value of ∼123 ms. We also estimate for the first time event durations of soft gamma repeater (SGR) bursts in photon space (i.e., using their deconvolved spectra) and find that these are very similar to the T 90 values estimated in count space (following a log-normal distribution with a mean value of ∼124 ms). We fit the time-integrated spectra for each burst and the time-resolved spectra of the five brightest bursts with several models. We find that a single power law with an exponential cutoff model fits all 29 bursts well, while 18 of the events can also be fit with two blackbody functions. We expand on the physical interpretation of these two models and we compare their parameters and discuss their evolution. We show that the time-integrated and time-resolved spectra reveal that E peak decreases with energy flux (and fluence) to a minimum of ∼30 keV at F = 8.7 × 10 −6 erg cm −2 s −1 , increasing steadily afterward. Two more sources exhibit a similar trend: SGRs J1550-5418 and 1806-20. The isotropic luminosity, L iso , corresponding to these flux values is roughly similar for all sources (0.4-1.5 × 10 40 erg s −1 ).

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Konus-Wind Observations of the New Soft Gamma-Ray Repeater SGR 0501+4516

Cited by 29 publications

References 26 publications

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

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

Pulsars and Magnetars

Fermi/GAMMA-RAY BURST MONITOR OBSERVATIONS OF SGR J0501+4516 BURSTS

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