3XMM J185246.6+003317: ANOTHER LOW MAGNETIC FIELD MAGNETAR

@article{Rea20143XMMJA,
  title={3XMM J185246.6+003317: ANOTHER LOW MAGNETIC FIELD MAGNETAR},
  author={Nanda Rea and Daniele Vigan{\`o} and Gian Luca Israel and Jos{\'e} A. Pons and Diego F. Torres},
  journal={The Astrophysical Journal},
  year={2014},
  volume={781}
}
N.R. is supported by a Ramon y Cajal fellowship and by an NWO Vidi award. N.R., D.V., and D.F.T. acknowledge support from grants AYA2012-39303, SGR 2009-811, and iLINK 2011-0303. J.A.P. acknowledges support from the grants AYA 2010-21097-C03-02 and Prometeo/2009/103. 

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References

SHOWING 1-10 OF 28 REFERENCES
THE OUTBURST DECAY OF THE LOW MAGNETIC FIELD MAGNETAR SGR 0418+5729
N.R. is supported by a Ramon y Cajal Research Fellowship, and by grants AYA2009-07391, AYA2012-39303, SGR2009-811, TW2010005, and iLINK 2011-0303. J.A.P. and D.V. acknowledge support from the grants
Spin-Down Measurement of PSR J1852+0040 in Kesteven 79: Central Compact Objects as Anti-Magnetars
Using XMM-Newton and Chandra, we achieved phase-connected timing of the 105 ms X-ray pulsar PSR J1852+0040 that provides the first measurement of the spin-down rate of a member of the class of
A new low magnetic field magnetar: the 2011 outburst of Swift J1822.3–1606
We report on the long-term X-ray monitoring withSwift,RXTE,Suzaku,Chandra, andXMM-Newton of the outburst of the newly discovered magnetar Swift J1822.3−1606 (SGR 1822−1606), from the first
DISCOVERY OF THE TRANSIENT MAGNETAR 3XMM J185246.6+003317 NEAR SUPERNOVA REMNANT KESTEVEN 79 WITH XMM-NEWTON
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IS SGR 0418+5729 INDEED A WANING MAGNETAR?
SGR 0418+5729 is a transient soft gamma-ray repeater which underwent a major outburst in 2009 June, during which the emission of short bursts was observed. Its properties appeared quite typical of
Magnetars versus High Magnetic Field Pulsars: A Theoretical Interpretation of the Apparent Dichotomy
Highly magnetized neutron stars (NSs) are characterized by a bewildering range of astrophysical manifestations. Here, building on our simulations of the evolution of magnetic stresses in the NS crust
SGR 0418+5729: a small inclination angle resulting in a not so low dipole magnetic field?
The spin down behaviors of SGR 0418+5729 are investigated. The pulsar spin down model of Contopoulos & Spitkovsky (2006) is applied to SGR 0418+5729. It is shown that SGR 0418+5729 lies below the
A Low-Magnetic-Field Soft Gamma Repeater
TLDR
The magnetar population may include objects with a wider range of B-field strengths, ages, and evolutionary stages than observed so far, implying that this population is wider than was previously thought.
A Unified Model of the Magnetar and Radio Pulsar Bursting Phenomenology
Anomalous X-ray pulsars (AXPs) and soft gamma-ray repeaters (SGRs) are young neutron stars (NSs) characterized by high X-ray quiescent luminosities, outbursts, and, in the case of SGRs, sporadic
POST-OUTBURST X-RAY FLUX AND TIMING EVOLUTION OF SWIFT J1822.3–1606
Swift J1822.3–1606 was discovered on 2011 July 14 by the Swift Burst Alert Telescope following the detection of several bursts. The source was found to have a period of 8.4377 s and was identified as
...
1
2
3
...