The Long and the Short of Gamma‐Ray Bursts

Katz, J. I.; Canel, L. M.

doi:10.1086/178018

Cited by 82 publications

(84 citation statements)

References 20 publications

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“…Spectral evolution from hard to soft through bursts is more or less ubiquitous (Band 1997). Events lasting more than 10 s differ from the shorter ones on average (Katz & Canel 1996), which suggests that two or more mechanisms may be responsible (neutron star mergers, failed supernovae, hypernovae, )). One can define a wide variety of correlations among spectra, durations, fluences, substructure, and so forth (Horack & Hakkila 1997), though many of these are not very robust (Lee & Petrosian 1996).…”

Section: And All the Restmentioning

confidence: 99%

Astrophysics in 1997

Trimble¹,

McFadden²

1998

PUBL ASTRON SOC PAC

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ABSTRACT. Martian marvels, a gamma-ray burster with a redshift, Galileo converses with Ganymede, a record galactic redshift of 4.92, and much else. Fiscal 1997 was definitely an exciting year for astronomers. We have tried hard to hit all the obvious highlights, but also to report more gradual progress on traditional problems of understanding planets, stars, galaxies, and the universe. Though the year was saddened by the loss of many valued colleagues, we nevertheless indulge in occasional soupçons of frivolity.

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Section: And All the Restmentioning

confidence: 99%

Astrophysics in 1997

Trimble¹,

McFadden²

1998

PUBL ASTRON SOC PAC

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“…It has been suggested (Cline et al 1999) that the small group of GRBs with T 90 < 0.1 s form an additional category. The short GRBs have a higher value of V/V max (Katz & Canel 1996), a much smaller value of the spectral lag (Norris et al 2000), a pulse shape that depends on position in the burst (Gupta et al 2000) and a smaller space density than long GRBs (Schmidt 2001).…”

Section: Introductionmentioning

confidence: 99%

Temporal properties of the short gamma-ray bursts

McBreen

Quilligan

McBreen

et al. 2001

A&A

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Abstract.A temporal analysis has been performed on a sample of 100 bright gamma-ray bursts (GRBs) with T90 < 2 s from the BATSE Current Catalog. The GRBs were denoised using a median filter and subjected to an automated pulse selection algorithm as an objective way of identifing the effects of neighbouring pulses. The rise times, fall times, F W HM, pulse amplitudes and areas were measured and the frequency distributions are presented here. All are consistent with lognormal distributions. The distribution of time intervals between pulses is not random but consistent with a lognormal distribution. The time intervals between pulses and pulse amplitudes are highly correlated with each other. These results are in excellent agreement with a similar analysis that revealed lognormal distributions for pulse properties and correlated time intervals between pulses in bright GRBs with T90 > 2 s. The two sub-classes of GRBs appear to have the same emission mechanism which is probably caused by internal shocks. They may not have the same progenitors because of the generic nature of the fireball model.

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“…a NS-BH merger [96,97,98], where the neutron star is tidally disrupted before being swallowed by the hole; the merger of a White Dwarf (WD) with a black hole [99]; the coalescence of binary WDs [71,87,100,101]; or accretion induced collapse (AIC) of a NS [102,103], where the collapsing neutron star has too much angular momentum to collapse quietly into a black hole. In an alternative class of models, it is supposed that the compact objects are contained within a globular cluster, and that the binary system will evolve mainly through hardening of the binary through three-body interactions [104,105] or physical star-star collisions [106] rather than by pure gravitational wave emission.…”

Section: Bestiarymentioning

confidence: 99%

The Progenitors of Short Gamma-Ray Bursts

Ramírez-Ruiz¹

2006

AIP Conference Proceedings

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Abstract. Recent months have witnessed dramatic progress in our understanding of short γ-ray burst (SGRB) sources. There is now general agreement that SGRBs -or at least a substantial subset of them -are capable of producing directed outflows of relativistic matter with a kinetic luminosity exceeding by many millions that of active galactic nuclei. Given the twin requirements of energy and compactness, it is widely believed that SGRB activity is ultimately ascribable to a modest fraction of a solar mass of gas accreting onto a stellar mass black hole or to a precursor stage whose inevitable end point is a stellar mass black hole. Astrophysical scenarios involving the violent birth of a rapidly rotating neutron star, or an accreting black hole in a merging compact binary driven by gravitational wave emission are reviewed, along with other possible alternatives (collisions or collapse of compact objects). If a black hole lies at the center of this activity, then the fundamental pathways through which mass, angular momentum and energy can flow around and away from it play a key role in understanding how these prime movers can form collimated, relativistic outflows. Flow patterns near black holes accreting matter in the hypercritical regime, where photons are unable to provide cooling, but neutrinos do so efficiently, are discussed in detail, and we believe that they offer the best hope of understanding the central engine. On the other hand, statistical investigations of SGRB niches also furnish valuable information on their nature and evolutionary behavior. The formation of particular kinds of progenitor sources appears to be correlated with environmental effects and cosmic epoch. In addition, there is now compelling evidence for the continuous fueling of SGRB sources. We suggest here that the observed late flaring activity could be due to a secondary accretion episode induced by the delayed fall back of material dynamically stripped from a compact object during a merger or collision. Some important unresolved questions are identified, along with the types of observation that would discriminate among the various models. Many of the observed properties can be understood as resulting from outflows driven by hyperaccreting black holes and subsequently collimated into a pair of anti-parallel jets. It is likely that most of the radiation we receive is reprocessed by matter quite distant to the black hole; SGRB jets, if powered by the hole itself, may therefore be one of the few observable consequences of how flows near nuclear density behave under the influence of strong gravitational fields.

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The Long and the Short of Gamma‐Ray Bursts

Cited by 82 publications

References 20 publications

Astrophysics in 1997

Astrophysics in 1997

Temporal properties of the short gamma-ray bursts

The Progenitors of Short Gamma-Ray Bursts

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