A Low-Magnetic-Field Soft Gamma Repeater

Rea, N.; Esposito, P.; Turolla, R.; Israel, G. L.; Zane, S.; Stella, L.; Mereghetti, S.; Tiengo, A.; Götz, D.; Göǧüş, E.; Kouveliotou, C.

doi:10.1126/science.1196088

Cited by 326 publications

(428 citation statements)

References 23 publications

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“…This was quite unexpected because the fast spin-down rates of all the other transient AXPs/SGRs were always evident after only a few days of observations. The upper limit ofṖ<6×10 −15 s s −1 obtained after two years implied B d <7.5×10 12 G [160], an unprecedented value for a source showing all the typical characteristics of a magnetar. Only recently, thanks to a phase-coherent timing analysis of all the observations of SGR 0418+5729 spanning more than three years, it has been possible to measure its small spin-down of (4±1)×10 −15 s s −1 [162], which translates into a field B d =6×10 12 G.…”

Section: Magnetars With Low External Fieldmentioning

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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Section: Magnetars With Low External Fieldmentioning

confidence: 99%

Pulsars and Magnetars

Mereghetti

2013

Braz J Phys

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“…The radio detections of XTE J1810-197 and 1E 1547J1810-197 and 1E -54 (Camilo et al 2006J1810-197 and 1E , 2007 and the very low spin-down rate of SGR 0418+5729 (Rea et al 2010), implying a dipole field close to that of normal pulsars, are only a few examples.…”

Section: Introductionmentioning

confidence: 99%

The magnetar candidate AX J1818.8−1559

Mereghetti¹,

Esposito²,

Tiengo³

et al. 2012

A&A

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In October 2007, a hard X-ray burst was detected by the INTEGRAL satellite from a direction consistent with the position of AX J1818.8−1559, an X-ray source at low Galactic latitude discovered with the Advanced Satellite for Cosmology and Astrophysics (ASCA) satellite in 1996-1999. The short duration (0.8 s) and soft spectrum (power-law photon index of 3.0 ± 0.2) of the burst in the 20-100 keV range are typical of soft gamma-ray repeaters and anomalous X-ray pulsars. We report on the results of an observation of AX J1818.8−1559 obtained with the Suzaku satellite in October 2011. The source spectrum, a power-law with photon index ∼1.5, and flux (∼2 × 10 −12 erg cm −2 s −1 , 2-10 keV) did not show significant variations from those derived from archival data of various satellites obtained from 1993 to 2011. We discuss possible interpretations of the data for AX J1818.8−1559 and, based on its association with the INTEGRAL burst, we propose it as a new member of the small class of magnetar candidates.

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“…Observationally, all known magnetars are X-ray pulsars with luminosities of L X ∼ (10 32 ∼ 10 36 ) erg s −1 (Rea et al 2010), their high luminosities together with the lack of evidence for ac-cretion from a stellar companion, result in the conclusion that the energy reservoir fueling the magnetar activity is their superhigh magnetic fields (10 14 ∼ 10 15 ) G (Dib et al 2008;Megreghetti 2008;Rea et al 2010). Such a huge energy reservoir (E ∼ 3×10 47 (B/10 15 G) 2 (R/10km) 3 erg) is sufficient to power not only the persistent surface Xray emission but also a steady stream of low-amplitude Alfven waves into the magnetosphere for ∼ 10 4 yrs (Thompson & Duncan 1995.…”

Section: Introductionmentioning

confidence: 99%

Evolution of superhigh magnetic fields of magnetars

Gao

Wang²,

Yuan³

et al. 2011

Astrophys Space Sci

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In this paper, we consider the effect of Landau levels on the decay of superhigh magnetic fields of magnetars. Applying 3 P 2 anisotropic neutron superfluid theory yield a second-order differential equation for a superhigh magnetic field B and its evolutionary timescale t. The superhigh magnetic fields may evolve on timescales ∼ (10 6 − 10 7 ) yrs for common magnetars. According to our model, the activity of a magnetar may originate from instability caused by the high electron Fermi energy.

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A Low-Magnetic-Field Soft Gamma Repeater

Cited by 326 publications

References 23 publications

Pulsars and Magnetars

Pulsars and Magnetars

The magnetar candidate AX J1818.8−1559

Evolution of superhigh magnetic fields of magnetars

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