The protomagnetar model for gamma-ray bursts

Metzger, Brian D.; Giannios, Dimitrios; Thompson, Todd A.; Bucciantini, N.; Quataert, Eliot

doi:10.1111/j.1365-2966.2011.18280.x

Cited by 661 publications

(713 citation statements)

References 252 publications

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“…Magnetic reconnection-driven multiple explosions then occur, producing X-ray flares. Some internal dissipations of relativistic winds from postburst millisecond magnetars (a type of pulsar with a magnetic field strength of ∼ 10 14 − 10 15 Gauss) could also lead to X-ray flares 12 . Furthermore, relativistic shells could be ejected from long-term hyperaccreting disks around stellar-mass black holes by some mechanism, for example the magnetic barrier effect 13 .…”

Section: Lines Inmentioning

confidence: 99%

“…Interestingly, 1 School of Astronomy and Space Science, Nanjing University, Nanjing 210093, China, 2 Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing 210093, China. *e-mail: fayinwang@nju.edu.cn; dzg@nju.edu.cn some theoretical models have suggested that GRB X-ray flares could be magnetically dominated explosive events [11][12][13] . However, a physical analogy between GRB X-ray flares and solar flares has not yet been established.…”

mentioning

confidence: 99%

“…some theoretical models have suggested that GRB X-ray flares could be magnetically dominated explosive events [11][12][13] . However, a physical analogy between GRB X-ray flares and solar flares has not yet been established.…”

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confidence: 99%

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Self-organized criticality in X-ray flares of gamma-ray-burst afterglows

2013

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X-ray flares detected in nearly half of gamma-ray-burst (GRB) afterglows are one of the most intriguing phenomena in highenergy astrophysics 1-8 . All of the observations indicate that the central engines of bursts, after the gamma-ray emission has ended, still have long periods of activity, during which energetic explosions eject relativistic materials, leading to late-time X-ray emission 2,9,10 . It is thus expected that X-ray flares provide important clues as to the nature of the central engines of GRBs, and more importantly, unveil the physical mechanism of the flares themselves, which has so far remained mysterious. Here we report statistical results of X-ray flares of GRBs with known redshifts, and show that X-ray flares and solar flares share three statistical properties: power-law frequency distributions for energies, durations and waiting times. All of the distributions can be well understood within the physical framework of a self-organized criticality (SOC) system. The statistical properties of X-ray flares of GRBs are similar to solar flares, and thus both can be attributed to a SOC process. Both types of flares may be driven by a magnetic reconnection process, but X-ray flares of GRBs are produced in ultra-strongly magnetized millisecond pulsars 11,12 or long-term hyperaccreting disks around stellar-mass black holes 13 .GRBs are flashes of gamma-rays occurring at cosmological distances with an isotropic-equivalent energy release from 10 51 to 10 54 ergs 9,10,14,15 . They can be sorted into two classes: shortduration hard-spectrum bursts (< 2 s) and long-duration softspectrum bursts 16 . Thanks to the rapid-response capability and high sensitivity of the Swift satellite 17 , numerous unforeseen features have been discovered, one of which is that about half of the bursts have large, late-time X-ray flares with short rise and decay times 4,5 . Unexpected X-ray flares with an isotropicequivalent energy from 10 48 to 10 52 ergs have been detected for both long and short bursts 4,6,7 . The occurrence times of X-ray flares range from a few seconds to 10 6 seconds after the GRB trigger 8 . Until now, the physical mechanism of X-ray flares has remained mysterious, although some models have been proposed 9,10 . Due to the 8-year observations of Swift, plentiful X-ray flare data have been collected. Here we investigate the frequency distributions of energies, durations and waiting times of GRB X-ray flares for the first time. On the other hand, it is well known that solar flares with a timescale of hours are explosive phenomena in the solar atmosphere with an energy release of about 10 28 -10 32 ergs, which are widely believed to be triggered by a magnetic reconnection process 18 . They have been observed in broadband electromagnetic waves, but we focus here on solar hard X-ray flares.Although X-ray flares are common phenomena in GRBs and the Sun, the flare energy spans about 20 orders of magnitude and an outstanding question appears, namely, do GRB X-ray flares and solar flares have a similar physical mechani...

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Section: Lines Inmentioning

confidence: 99%

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confidence: 99%

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Self-organized criticality in X-ray flares of gamma-ray-burst afterglows

2013

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“…In a more evolved version of this model, the magnetic field B decays with time as the angular speed. [4] found that, for an initial period P ≃ 1 ms and B ≃ 10 15 G, the jet luminosity, decay slope and duration are similar to those observed for GRB 130831A. The expected collapse of the magnetar into a BH, for the P and B parameters above, should take ≃ 60 ks (cosmological frame), again quite similar to the case of GRB 130831A.…”

Section: Origin Of the Emission: Forward Shock (Fs) And Internal Dissmentioning

confidence: 55%

GRB 130831A: The Birth and Death of a Magnetar at z=0.5

Pasquale¹,

Oates²,

Racusin³

et al. 2015

Proceedings of Swift: 10 Years of Discovery — PoS(SWIFT 10)

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“…For long GRBs, the main models for a central engine that is powering the GRB include the popular collapsar model (Woosley 1993;MacFadyen & Woosley 1999) and the magnetar model (e.g., Usov 1992, for a good summary see Metzger et al 2010), while rapid rotation of the pre-explosion stellar core appears to be a necessary ingredient for both scenarios.…”

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confidence: 99%

Stellar Forensics with the Supernova‐GRB Connection

Modjaz¹

2011

Reviews in Modern Astronomy

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Long-duration gamma-ray bursts (GRBs) and Type Ib/c Supernovae (SNe Ib/c) are amongst nature's most magnificent explosions. While GRBs launch relativistic jets, SNe Ib/c are core-collapse explosions whose progenitors have been stripped of their hydrogen and helium envelopes. Yet for over a decade, one of the key outstanding questions is which conditions lead to each kind of explosion and death in massive stars. Determining the fates of massive stars is not only a vibrant topic in itself, but also impacts using GRBs as star formation indicators over distances of up to 13 billion light-years and for mapping the chemical enrichment history of the universe. This article reviews a number of comprehensive observational studies that probe the progenitor environments, their metallicities and the explosion geometries of SN with and without GRBs, as well as the emerging field of SN environmental studies. Furthermore, it discusses SN 2008D/XRT 080109 which was discovered serendipitously with the Swift satellite via its X-ray emission from shock breakout, and which has generated great interest amongst both observers and theorists while illustrating a novel technique for stellar forensics. The article concludes with an outlook on how the most promising venues of research -with the many existing and upcoming large-scale surveys such as the Palomar Transient Factory and LSST -will shed new light on the diverse deaths of massive stars.

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The protomagnetar model for gamma-ray bursts

Cited by 661 publications

References 252 publications

Self-organized criticality in X-ray flares of gamma-ray-burst afterglows

Self-organized criticality in X-ray flares of gamma-ray-burst afterglows

GRB 130831A: The Birth and Death of a Magnetar at z=0.5

Stellar Forensics with the Supernova‐GRB Connection

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