Detection of a fast, intense and unusual gamma-ray transient

Cline, T. L.; Desai, U. D.; Pizzichini, G.; Teegarden, B. J.; Evans, W. D.; Klebesadel, R. W.; Laros, J. G.; Hurley, K.; Niel, M.; Védrenne, G.

doi:10.1086/183221

Cited by 141 publications

(66 citation statements)

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“…Refs. -(1) Barthelmy et al (2008); (2) Göǧüş et al (2010); (3) Gaensler & Chatterjee (2008); (4) Leahy & Tian (2007); (5) Mezets et al (1979); (6) Cline et al (1980); (7) Park et al (2012); (8) Kouveliotou et al (1998); (9) Watcher et al (2004); (10) Corbel et al (1999); (11) Sarma et al (1997); (12) Vasisht & Gotthelf (1997); (17) Tendulkar (2013); (18) ; (19) Fahlman & Gregory (1981); (20) Tendulkar et al (2013); (21) Kothes & Foster (2012); (22) Gotthelf & Vasisht (1998); (23) Gaensler et al (1999); (24) Vasisht et al (2000); 25 Torii et al (1998); (27) Halpern & Gotthelf (2010); (28) Tian & Leahy (2012); (26) Aharonian et al (2008); (29) Levin et al (2010); (30) Anderson et al (2012); (31) Gotthelf et al (2000); (32) Leahy & Tian (2008b); (33) Gelfand et al (20...…”

Section: Introductionmentioning

confidence: 99%

Learning about the magnetar Swift J1834.9−0846 from its wind nebula

Granot

Gill

Younes

et al. 2016

Mon. Not. R. Astron. Soc.

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The first wind nebula around a magnetar was recently discovered in X-rays around Swift J1834.9−0846. We study this magnetar's global energetics and the properties of its particle wind or outflows. At a distance of ∼ 4 kpc, Swift J1834.9−0846 is located at the center of the supernova remnant (SNR) W41 whose radius is ∼ 19 pc, an order of magnitude larger than that of the X-ray nebula (∼ 2 pc). The association with SNR W41 suggests a common age of ∼ 5−100 kyr, while its spin-down age is 4.9 kyr. A small natal kick velocity may partly explain why a wind nebula was detected around this magnetar but not around other magnetars, most of which appear to have larger kick velocities and may have exited their birth SNR. We find that the GeV and TeV source detected by Fermi/LAT and H.E.S.S., respectively, of radius ∼ 11 pc is most likely of hadronic origin. The dynamics and internal structure of the nebula are examined analytically to explain the nebula's current properties. Its size may naturally correspond to the diffusion-dominated cooling length of the X-ray emitting e + e − pairs. This may also account for the spectral softening of the X-ray emission from the nebula's inner to outer parts. Analysis of the X-ray synchrotron nebula implies that (i) the nebular magnetic field is 11 µG (and likely 30 µG), and (ii) the nebula is not powered predominantly by the magnetar's quiescent spin-down-powered MHD wind, but by other outflows that contribute most of its energy. The latter are most likely associated with the magnetar's bursting activity, and possibly dominated by outflows associated with its past giant flares. The energy source for the required outflows cannot be the decay of the magnetar's dipole field alone, and is most likely the decay of its much stronger internal magnetic field.

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Section: Introductionmentioning

confidence: 99%

Learning about the magnetar Swift J1834.9−0846 from its wind nebula

Granot

Gill

Younes

et al. 2016

Mon. Not. R. Astron. Soc.

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“…B 10 15 G. They argue that the 5 March burst was due to a large-scale readjustment of the stellar magnetic field, while the more standard SGR bursts are caused by the release of magnetic stresses within a more localized patch of the crust. Thompson & Duncan put forth a variety of independent arguments in favour of the magnetar scenario, including (i) the necessity of a very high B-field to spin down the pulsar to 8 s within the inferred 10 4 year age of N49, (ii) a very strong B-field suppresses the e − -scattering cross section below the standard Thomson value by the ratio (B/B QED ) −2 , where B QED = m 2 e c 2 /(eh) = 4.4 × 10 13 G (the point at which the non-relativistic Landau energyheB/(m e c) equals the electron rest energy m e c 2 ), therefore enabling L 10 4 L Edd for surface fields 10 14.5 G, (iii) persistent X-ray emission from SGR 0526-66 at 7 × 10 35 erg s −1 [25,26] implies B crust 10 15 G, and (iv) an identification of the 0.15 s duration of the hard spike of the March 5th event [23,27] with the internal Alfvén crossing time leads to B 7 × 10 14 G.…”

Section: The Modern Era (A) Missionsmentioning

confidence: 99%

High-energy transients

Gehrels

Cannizzo

2013

Phil. Trans. R. Soc. A.

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We present an overview of high-energy transients in astrophysics, highlighting important advances over the past 50 years. We begin with early discoveries of γ-ray transients, and then delve into physical details associated with a variety of phenomena. We discuss some of the unexpected transients found by Fermi and Swift, many of which are not easily classifiable or in some way challenge conventional wisdom. These objects are important insofar as they underscore the necessity of future, more detailed studies.

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“…Soft gamma-ray repeaters emitting energetic photons up to several million electron volts represent another example of violent explosions associated with neutron stars [27,28]. These sources rise on time scales of a fraction of a second to peak luminosities approximately 10 45 ergs s −1 that radiate most of the energy.…”

Section: (B) Neutron Star and Black Hole Binary Transientsmentioning

confidence: 99%

Astrophysical explosions: from solar flares to cosmic gamma-ray bursts

Wheeler

2012

Phil. Trans. R. Soc. A.

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Astrophysical explosions result from the release of magnetic, gravitational or thermonuclear energy on dynamical time scales, typically the sound-crossing time for the system. These explosions include solar and stellar flares, eruptive phenomena in accretion discs, thermonuclear combustion on the surfaces of white dwarfs and neutron stars, violent magnetic reconnection in neutron stars, thermonuclear and gravitational collapse supernovae and cosmic gamma-ray bursts, each representing a different type and amount of energy release. This paper summarizes the properties of these explosions and describes new research on thermonuclear explosions and explosions in extended circumstellar media. Parallels are drawn between studies of terrestrial and astrophysical explosions, especially the physics of the transition from deflagration-to-detonation.

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Detection of a fast, intense and unusual gamma-ray transient

Cited by 141 publications

References 0 publications

Learning about the magnetar Swift J1834.9−0846 from its wind nebula

Learning about the magnetar Swift J1834.9−0846 from its wind nebula

High-energy transients

Astrophysical explosions: from solar flares to cosmic gamma-ray bursts

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