Is SGR 0418+5729 Indeed a Waning Magnetar?

Turolla, R.; Zane, S.; Pons, José A.; Esposito, P.; Rea, N.

doi:10.1088/0004-637x/740/2/105

Cited by 86 publications

(118 citation statements)

References 44 publications

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“…As argued in more detail in Rea et al (2012), we note that the discovery of a second magnetar-like source with a magnetic field in the radio-pulsar range strengthens the idea that magnetar-like behavior may be much more widespread than what believed in the past, and that it is related to the intensity and topology of the internal and surface toroidal components, rather than only to the surface dipolar field (Rea et al 2010, Perna & Pons 2011, Turolla et al 2011.…”

Section: Discussionsupporting

confidence: 74%

A new low-B magnetar: Swift J1822.3–1606

Camero-Arranz¹,

Rea²,

Israel

et al. 2012

Proc. IAU

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We report on the long term X-ray monitoring with Swift, RXTE, Suzaku, Chandra, and XMM-Newton of the outburst of the newly discovered magnetar Swift J1822.3–1606 (SGR 1822-1606), from the first observations soon after the detection of the short X-ray bursts which led to its discovery (July 2011), through the first stages of its outburst decay (April 2012). Our X-ray timing analysis finds the source rotating with a period of P = 8.43772016(2) s and a period derivative Ṗ = 8.3(2) × 10−14 ss−1, which entails an inferred dipolar surface magnetic field of B ≃ 2.7 × 1013 G at the equator. This measurement makes Swift J1822.3–1606 the second lowest magnetic field magnetar (after SGR 0418+5729; Rea et al. 2010). Following the flux and spectral evolution from the beginning of the outburst, we find that the flux decreased by about an order of magnitude, with a subtle softening of the spectrum, both typical of the outburst decay of magnetars. By modeling the secular thermal evolution of Swift J1822.3–1606, we find that the observed timing properties of the source, as well as its quiescent X-ray luminosity, can be reproduced if it was born with a poloidal and crustal toroidal fields of Bp ~ 1.5 × 1014 G and Btor ~ 7 × 1014 G, respectively, and if its current age is ~550 kyr (Rea et al. 2012).

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Section: Discussionsupporting

confidence: 74%

A new low-B magnetar: Swift J1822.3–1606

Camero-Arranz¹,

Rea²,

Israel

et al. 2012

Proc. IAU

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“…∼ 6 × 10 12 G; Rea et al 2013). Simulations of magnetic field evolution in neutron stars with different initial field strength and configuration have shown that, a relatively old magnetar such as SGR 0418+5729 despite its low surface dipolar field, might still harbor a sufficiently intense internal/crustal toroidal field to give rise to outbursts and short X-ray bursts (Turolla et al 2011).…”

Section: Introductionmentioning

confidence: 99%

The outburst decay of the low magnetic field magnetar SWIFT J1822.3−1606: phase-resolved analysis and evidence for a variable cyclotron feature

Castillo

Israel

Tiengo

et al. 2016

Mon. Not. R. Astron. Soc.

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“…The decay rate of the dipole field depends mainly on the strength of the initial crustal toroidal arXiv:1412.1677v2 [astro-ph.HE] 11 Jan 2015 field. For instance, for a neutron star to reach the properties of the so-called low-B magnetar SGR 0418+5729, it should have an initial toroidal field stronger than 10 16 G (Turolla et al 2011). For a second low-B magnetar Swift J1822.3-1606, the model needs an initial crustal toroidal field with a strength of a few 10 14 G.…”

Section: Introductionmentioning

confidence: 99%

Long-term evolution, X-ray outburst and optical/infrared emission of SGR 0501+4516

Benli

Çalışkan

Ertan

2015

Monthly Notices of the Royal Astronomical Society

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We have analyzed the long-term evolution and the X-ray outburst light curve of SGR 0501+4516 in the frame of the fallback disc model. We have shown that the X-ray luminosity, period and period derivative of this typical soft gamma repeater can be achieved by a neutron star with a large range of initial disc masses provided that the source has a magnetic dipole field of ∼ 1.4 × 10 12 G on the pole of the star. At present, the star is accreting matter from the disc, which has an age ∼ 3 × 10 4 yr, and will remain in the accretion phase until t ∼ 2-5 × 10 5 yr depending on the initial disc mass. With its current rotational rate, this source is not expected to give pulsed radio emission even if the accretion on to the star is hindered by some mechanism. The X-ray enhancement light curve of SGR 0501+4516 can be accounted for by the same model applied earlier to the X-ray enhancement light curves of other anomalous X-ray pulsars/soft gamma repeaters with the same basic disc parameters. We have further shown that the optical/IR data of SGR 0501+4516 is in good agreement with the emission from an irradiated fallback disc with the properties consistent with our long-term evolution model.

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Is SGR 0418+5729 Indeed a Waning Magnetar?

Cited by 86 publications

References 44 publications

A new low-B magnetar: Swift J1822.3–1606

A new low-B magnetar: Swift J1822.3–1606

The outburst decay of the low magnetic field magnetar SWIFT J1822.3−1606: phase-resolved analysis and evidence for a variable cyclotron feature

Long-term evolution, X-ray outburst and optical/infrared emission of SGR 0501+4516

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