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:10.1007/978-94-009-7960-4

Cited by 38 publications

(32 citation statements)

References 2 publications

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“…KONUS SHBwEE. This shows three of the best examples of SHBwEE from the KONUS catalogue (Mazets et al 2002). These three bursts also show the profile of initial spike, followed by a hiatus of emission, then increasing soft emission, peaking and then decreasing emission.…”

Section: (C ) the Horvath Third Class Of Burstsmentioning

confidence: 70%

“…Figure 11 shows three KONUS bursts that are clearly in the same SHBwEE temporal and spectral envelope. Additionally, KONUS has six more bursts with nearly the same signature (Mazets et al 2002)-the only difference is that there is no clear hiatus of emission immediately after the initial spike. Given that four instruments have seen these SHBwEEs and at least one BAT SHBwEE would have been classified as a traditional SHB (i.e.…”

Section: Short Hard Bursts With Extended Emissionmentioning

confidence: 99%

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Swift-BAT results on the prompt emission of short bursts

Barthelmy

2007

Phil. Trans. R. Soc. A.

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This is a brief review of short hard bursts (SHBs) from previous missions and from Swift-BAT; in particular, a review of the developing class of gamma-ray bursts which are similar to SHBs in that they have the short hard initial spike (0.1 to a few seconds), but that they also have a long extended phase of soft emission (50-200 s). Further, we suggest that a class of events discovered by Horvath in the T90 versus hardness ratio plane is this SHB with extended emission.

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Section: (C ) the Horvath Third Class Of Burstsmentioning

confidence: 70%

Section: Short Hard Bursts With Extended Emissionmentioning

confidence: 99%

Swift-BAT results on the prompt emission of short bursts

Barthelmy

2007

Phil. Trans. R. Soc. A.

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“…The detection and localization of GRBs by the BDRG is based on the design of the KONUS instrument, which utilized three omni-directional detectors with axes set normal to each other (see Fig. 1) (Mazets et al 1981). The Konus device was operated successfully onboard the Venus 11-14 interplanetary stations and on the KONUS-Wind mission.…”

Section: Observations With Bdrg Gamma Ray Burst Monitormentioning

confidence: 99%

Wide-Field Gamma-Spectrometer BDRG: GRB Monitor On-Board the Lomonosov Mission

et al. 2017

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The study of GRB prompt emissions (PE) is one of the main goals of the Lomonosov space mission. The payloads of the GRB monitor (BDRG) with the widefield optical cameras (SHOK) and the ultra-fast flash observatory (UFFO) onboard the Lomonosov satellite are intended for the observation of GRBs, and in particular, their prompt emissions. The BDRG gamma-ray spectrometer is designed to obtain the temporal and spectral information of GRBs in the energy range of 10-3000 keV as well as to provide GRB triggers on several time scales (10 ms, 1 s and 20 s) for ground and space telescopes, including the UFFO and SHOK. The BDRG instrument consists of three identical detector boxes with axes shifted by 90 • from each other. This configuration allows us to localize a GRB source in the sky with an accuracy of ∼ 2 • .Each BDRG box contains a phoswich NaI(Tl)/CsI(Tl) scintillator detector. A thick CsI(Tl) crystal in size of ∅130 × 17 mm is placed underneath the NaI(Tl) as an active shield in the soft energy range and as the main detector in the hard energy range. The ratio of the CsI(Tl) to NaI(Tl) event rates at varying energies can be employed as an independent metric to distinguish legitimate GRB signals from false positives originating from electrons in near-Earth vicinities.The data from three detectors are collected in a BA BDRG information unit, which generates a GRB trigger and a set of data frames in output format. The scientific data output is ∼ 500 Mb per day, including ∼ 180 Mb of continuous data for events with durations in excess of 100 ms for 16 channels in each detector, detailed energy spectra, and sets of frames with ∼ 5 Mb of detailed information for each burst-like event. A number of pre-flight tests including those for the trigger algorithm and calibration were carried out to confirm the reliability of the BDRG for operation in space.

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“…Besides viscosity and radiation which can damp the ellipsoid-like motions and allow collapse, there is the possibility that inertial interactions with higher order modes that must be present in the real stratified bodies may cause an inertial cascade and drain the energy from the sec-ond order modes an a non-secular way that does not depend on dissipative coefficients. It is very seductive to connect chaotic oscillations with highly variable emission observed in the prompt gamma ray emission of cosmic gamma ray bursts (Mazets et al 1981). A presence of rotation and magnetic field strongly complicate the picture of the core-collapse supernova explosion (Ardeljan, Bisnovatyi-Kogan & Moiseenko 2005;Moiseenko, Bisnovatyi-Kogan & Ardeljan 2005).…”

Section: Investigation Of Regular and Chaotic Oscillations Via The Pomentioning

confidence: 99%

Regular and chaotic dynamics of non-spherical bodies. Zeldovich’s pancakes and emission of very long gravitational waves

Бисноватый-Коган

Tsupko

2015

J. Plasma Phys.

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In this paper we review a recently developed approximate method for investigation of dynamics of compressible ellipsoidal figures. Collapse and subsequent behaviour are described by a system of ordinary differential equations for time evolution of semi-axes of a uniformly rotating, three-axis, uniform-density ellipsoid. First, we apply this approach to investigate dynamic stability of non-spherical bodies. We solve the equations that describe, in a simplified way, the Newtonian dynamics of a self-gravitating non-rotating spheroidal body. We find that, after loss of stability, a contraction to a singularity occurs only in a pure spherical collapse, and deviations from spherical symmetry prevent the contraction to the singularity through a stabilizing action of nonlinear non-spherical oscillations. The development of instability leads to the formation of a regularly or chaotically oscillating body, in which dynamical motion prevents the formation of the singularity. We find regions of chaotic and regular pulsations by constructing a Poincar diagram. A real collapse occurs after damping of the oscillations because of energy losses, shock wave formation or viscosity. We use our approach to investigate approximately the first stages of collapse during the large scale structure formation. The theory of this process started from ideas of Ya. B. Zeldovich, concerning the formation of strongly non-spherical structures during nonlinear stages of the development of gravitational instability, known as 'Zeldovich's pancakes'. In this paper the collapse of non-collisional dark matter and the formation of pancake structures are investigated approximately. Violent relaxation, mass and angular momentum losses are taken into account phenomenologically. We estimate an emission of very long gravitational waves during the collapse, and discuss the possibility of gravitational lensing and polarization of the cosmic microwave background by these waves.

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Catalog of Cosmic Gamma-Ray Bursts from the KONUS Experiment Data

Cited by 38 publications

References 2 publications

Swift-BAT results on the prompt emission of short bursts

Swift-BAT results on the prompt emission of short bursts

Wide-Field Gamma-Spectrometer BDRG: GRB Monitor On-Board the Lomonosov Mission

Regular and chaotic dynamics of non-spherical bodies. Zeldovich’s pancakes and emission of very long gravitational waves

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