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/bf00649140

Cited by 296 publications

(113 citation statements)

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“…Short GRBs are traditionally defined as those with durations of t 90 < 2 s. Observations with Konus and BATSE suggested they form a separate population from the long GRBs, and so may well also have different progenitors (Mazets et al 1981(Mazets et al , 1982Kouveliotou et al 1993). Following the identification of supernovae signatures in the afterglows of long GRBs, the favoured model for short bursts rapidly became the merger of two compact objects (neutron star-neutron star or neutron star-black hole), a model which had previously been popular for the long GRB population (e.g.…”

Section: Defining Short Grbsmentioning

confidence: 99%

“…Mazets et al 1981Mazets et al , 1982. This difference, secured by observations with BATSE in the 1990s (Kouveliotou et al 1993), led to the identification of short and long duration GRBs, one with a typical duration (normally defined as t 90 , the time over which 90 % of the total energy release in γ -rays is recorded) of around 1 s, and the other with a characteristic duration of about a minute.…”

Section: Introductionmentioning

confidence: 99%

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Gamma-Ray Burst Progenitors

et al. 2016

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We review our current understanding of the progenitors of both long and short duration gamma-ray bursts (GRBs). Constraints can be derived from multiple directions, and we use three distinct strands; (i) direct observations of GRBs and their host galaxies, (ii) parameters derived from modelling, both via population synthesis and direct numerical simulation and (iii) our understanding of plausible analog progenitor systems observed in the local Universe. From these joint constraints, we describe the likely routes that can drive massive stars to the creation of long GRBs, and our best estimates of the scenarios that can create compact object binaries which will ultimately form short GRBs, as well as the associated rates of both long and short GRBs. We further discuss how different the progenitors may be in the case of black hole engine or millisecond-magnetar models for the production of GRBs, and how central engines may provide a unifying theme between many classes of extremely luminous transient, from luminous and super-luminous supernovae to long and short GRBs.

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Section: Defining Short Grbsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Gamma-Ray Burst Progenitors

et al. 2016

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“…SGR 1806-20 was observed by Mazets et al in 1980 [61, 62], and was identified as SGR in [49] (Giant burst happened at 27 December 2006, with total energy ∼ 2 · 10 46 erg [61,62]). …”

Section: Giant Burstsmentioning

confidence: 99%

Evolutions of Neutron Stars and their Magnetic Fields

Бисноватый-Коган¹

2018

Proceedings of XII Multifrequency Behaviour of High Energy Cosmic Sources Workshop — PoS(MULTIF2017)

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Estimations of magnetic fields of neutron stars, observed as radio and X-ray pulsars, are discussed. It is shown, that theoretical and observational values for different types of radio pulsars are in good correspondence. Radio pulsars in close binaries and millisecond pulsars, which have passed the stage of disk accretion (recycled radio pulsars), have magnetic fields 2-4 orders of magnitude smaller than ordinary single pulsars. Most probably, the magnetic field of the neutron star was screened by the infalling material. Several screening models are considered. Formation of single recycled pulsars loosing its companion is discussed. Magnetic fields of some X-ray pulsars are estimated from the cyclotron line energy. In the case of Her X-1 this estimation exceeds considerably the value of its magnetic field obtained from long term observational data related to the beam structure evolution. Another interpretation of the cyclotron feature, based on the relativistic dipole radiation mechanism, could remove this discrepancy. Observational data about soft gamma repeaters and their interpretation as magnetars are critically analyzed.

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“…Gamma-ray bursts (GRBs) are traditionally classified based on their duration [1][2][3][4][5]: short GRBs last 2 s, while long GRBs last 2 s.…”

Section: Introductionmentioning

confidence: 99%

What can we learn from GRBs?

et al. 2018

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Abstract. We review our recent results on the classification of long and short gamma-ray bursts (GRBs) in different subclasses. We provide observational evidences for the binary nature of GRB progenitors. For long bursts the induced gravitational collapse (IGC) paradigm proposes as progenitor a tight binary system composed of a carbon-oxygen core (CO core ) and a neutron star (NS) companion; the supernova (SN) explosion of the CO core triggers a hypercritical accretion process onto the companion NS. For short bursts a NS-NS merger is traditionally adopted as the progenitor. We also indicate additional sub-classes originating from different progenitors: (CO core )-black hole (BH), BH-NS, and white dwarf-NS binaries. We also show how the outcomes of the further evolution of some of these sub-classes may become the progenitor systems of other sub-classes.

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

Cited by 296 publications

References 1 publication

Gamma-Ray Burst Progenitors

Gamma-Ray Burst Progenitors

Evolutions of Neutron Stars and their Magnetic Fields

What can we learn from GRBs?

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