Catalog of cosmic gamma-ray bursts from the KONUS experiment data

Mazets, E.; Golenetskii, S.; Ilyinskii, V. N.; Панов, В. Н.; Aptekar, R.; Gur’yan, Yu. A.; Proskura, M. P.; Соколов, И. А.; Sokolova, Z. Ya.; Харитонова, Т. В.; Dyatchkov, A.; Khavenson, N.

doi:10.1007/bf00649142

Cited by 45 publications

(24 citation statements)

References 6 publications

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“…The time‐scale of the prompt emission lasts from a few milliseconds (Vedrenne 1981) to thousands of seconds (Hurley, Sari & Djorgovski 2002). The distribution of its duration has been shown to be bimodal (Mazets et al 1981; Norris et al 1984; Hurley 1989; Dezalay et al 1992; Kouveliotou et al 1993); therefore GRBs can be classified as ‘short’ and ‘long’. The time profile of the prompt emission may present either multiple spikes of very short duration or relatively broad peaks with no fast variability (Norris et al 2005).…”

Section: Introductionmentioning

confidence: 99%

Unveiling the origin of X-ray flares in gamma-ray bursts

Chincarini¹,

Mao²,

Margutti³

et al. 2010

Monthly Notices of the Royal Astronomical Society

177

280

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We present an updated catalogue of 113 X-ray flares detected by Swift in the ~33 per cent of the X-ray afterglows of gamma-ray burst (GRB). 43 flares have a measured redshift. For the first time the analysis is performed in four different X-ray energy bands, allowing us to constrain the evolution of the flare temporal properties with energy. We find that flares are narrower at higher energies: their width follows a power-law relation w ~ E^(-0.5) reminiscent of the prompt emission. Flares are asymmetric structures, with a decay time which is twice the rise time on average. Both time-scales linearly evolve with time, giving rise to a constant rise-to-decay ratio: this implies that both time-scales are stretched by the same factor. As a consequence, the flare width linearly evolves with time to larger values: this is a key point that clearly distinguishes the flare from the GRB prompt emission. The flare 0.3-10 keV peak luminosity decreases with time, following a power-law behaviour with large scatter: Lpk ~ t^(-2.7+/-0.5). When multiple flares are present, a global softening trend is established: each flare is on average softer than the previous one. The 0.3-10 keV isotropic energy distribution is a lognormal peaked at 10^51 erg, with a possible excess at low energies. The flare average spectral energy distribution is found to be a power law with spectral energy index β ~ 1.1. These results confirmed that the flares are tightly linked to the prompt emission. However, after considering various models we conclude that no model is currently able to account for the entire set of observations

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Section: Introductionmentioning

confidence: 99%

Unveiling the origin of X-ray flares in gamma-ray bursts

Chincarini¹,

Mao²,

Margutti³

et al. 2010

Monthly Notices of the Royal Astronomical Society

177

280

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“…It has been recognized for a long time that the time duration of gamma-ray bursts (GRBs) is bimodal: the majority (75 per cent) of the bursts have a long duration with a mean of ∼20 s; the rest have a much shorter duration with a mean of only ∼0.2 s (Mazets et al 1981;Hurley et al 1992). Both of these two classes of GRBs have similar isotropic spatial distributions, but differ with respect to spectral hardness, fluence and temporal pulse properties (e.g.…”

Section: Introductionmentioning

confidence: 99%

Galactic distribution of merging neutron stars and black holes - prospects for short gamma-ray burst progenitors and LIGO/VIRGO

Voss¹,

Tauris²

2003

Monthly Notices of the Royal Astronomical Society

270

304

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We have performed a detailed population synthesis on a large number (2 × 107) of binary systems in order to investigate the properties of massive double degenerate binaries. We have included new important results in our input physics in order to obtain more reliable estimates of the merging time‐scales and relative formation rates. These improvements include refined treatment of the binding energy in a common envelope, helium star evolution and reduced kicks imparted to new‐born black holes. The discovery and observations of gamma‐ray burst afterglows and the identification of host galaxies have allowed comparisons of theoretical distributions of merger sites with the observed distribution of afterglow positions relative to host galaxies. To help investigate the physical nature of short‐ and long‐duration gamma‐ray bursts, we compute the distances of merging neutron stars (NS) and/or black holes (BH) from the centres of their host galaxies, as predicted by their formation scenario combined with motion in galactic potentials. Furthermore, we estimate the formation rate and merging rate of these massive double degenerate binaries. The latter is very important for the prospects of detecting gravitational waves with LIGO/VIRGO. We find that the expected detection rate for LIGO II is ∼850 yr−1 for galactic field sources and that this rate is completely dominated by merging double black hole (BHBH) binaries. Even LIGO I may detect such an event (∼0.25 yr−1). Our preferred model estimates the Galactic field double neutron star (NSNS) merger rate to be ∼1.5 × 10−6 yr−1. For BHBH systems this model predicts a merger rate of ∼9.7 × 10−6 yr−1. Our studies also reveal an accumulating numerous population of very wide‐orbit BHBH systems which never merge (τ≫τHubble).

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“…The detection of counterparts at other wavelengths for long duration GRBs, revealed their cosmological origin (see van Paradijs et al 2000, for a review) and it is accepted nowadays that they are associated with the death of massive stars. On the other hand, the nature of short duration GRBs, a class that comprises about 25% of all events (Mazets et al 1981;Kouveliotou et al 1993), still remains a puzzle. No counterparts have been discovered so far, in spite of intense efforts in order to detect the optical, infrared and radio Based on observations taken with the 1.2 m Mercator telescope at Observatorio del Roque de los Muchachos, with the 1.5 m telescope at Observatorio de Sierra Nevada, with the 2.2 m and 3.5 m telescopes at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto (operated jointly by the Max-Planck Institut für Astronomie and the Instituto de Astrofísica de Andalucía (CSIC)) and with the 6.0 m telescope at the Special Astrophysical Observatory in Russia. counterparts to several short, hard bursts (Kehoe et al 2001;Gorosabel et al 2002;Hurley et al 2002;Klotz et al 2003).…”

Section: Introductionmentioning

confidence: 99%

GRB 050509b: the elusive optical/nIR/mm afterglow of a short-duration GRB

Castro-Tirado

Postigo

Gorosabel

et al. 2005

A&A

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Abstract. We present multiwavelength (optical/near infrared/millimetre) observations of a short duration gamma-ray burst detected by Swift (GRB 050509b) collected between 0 seconds and ∼18.8 days after the event. No optical, near infrared or millimetre emission has been detected in spite of the well localised X-ray afterglow, confirming the elusiveness of the short duration events. We also discuss the possibility of the burst being located in a cluster of galaxies at z = 0.225 or beyond. In the former case, the spectral energy distribution of the neighbouring, potential host galaxy, favours a system harbouring an evolved dominant stellar population (age ∼360 Myr), unlike most long duration GRB host galaxies observed so far, i.e. thus giving support to a compact binary merger origin. Any underlying supernova that could be associated with this particular event should have been at least 3 magnitudes fainter than the type Ib/c SN 1998bw and 2.3 mag fainter than a typical type Ia SN.

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Catalog of cosmic gamma-ray bursts from the KONUS experiment data

Cited by 45 publications

References 6 publications

Unveiling the origin of X-ray flares in gamma-ray bursts

Unveiling the origin of X-ray flares in gamma-ray bursts

Galactic distribution of merging neutron stars and black holes - prospects for short gamma-ray burst progenitors and LIGO/VIRGO

GRB 050509b: the elusive optical/nIR/mm afterglow of a short-duration GRB

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