The 5 March 1979 event and the distinct class of short gamma bursts: are they of the same origin?

Mazets, E.; Golenetskii, S.; Gur’yan, Yu. A.; Ilyinskii, V. N.

doi:10.1007/bf00713635

Cited by 95 publications

(49 citation statements)

References 14 publications

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“…This result may be contrasted with that of Mazets et al (1982), who Ðtted an OTTB function to the energy spectra of the pulsating component of the March 5 burst. They found the interpulse spectra to be slightly softer, by 4 keV, than the pulse spectra.…”

Section: Reanalysis Of the Signe And Isee-3 Data On The March 5 Eventmentioning

confidence: 65%

The Giant Flare of 1998 August 27 from SGR 1900+14. I. An Interpretive Study ofBeppoSAXandUlyssesObservations

Feroci

Hurley

Duncan

et al. 2001

ApJ

127

172

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The giant Ñare of 1998 August 27 from SGR 1900]14 was extraordinary in many ways : it was the most intense Ñux of gamma rays ever detected from a source outside our solar system ; it was longer than any previously detected burst from a soft gamma repeater (SGR) in our Galaxy by more than an order of magnitude ; and it showed a remarkable four-peaked, periodic pattern in hard X-rays with the same rotation period that was found modulating soft X-rays from the star in quiescence. The event was detected by several gamma-ray experiments in space, including the Ulysses gamma-ray burst detector and the BeppoSAX Gamma-Ray Burst Monitor. These instruments operate in di †erent energy ranges, and comparisons of their measurements reveal complex patterns of spectral evolution as the intensity varies. In this paper, we present a joint analysis of the BeppoSAX and Ulysses data and discuss some implications of these results for the SGRs. We also present newly analyzed V enera/SIGNE and ISEE-3 data on the 1979 March 5 giant Ñare from an SGR in the Large Magellanic Cloud (SGR 0526[66) and compare them with the August 27 event. Our results are consistent with the hypothesis that giant Ñares are due to catastrophic magnetic instabilities in highly magnetized neutron stars, or "" magnetars.ÏÏ In particular, observations indicate that the initial hard spike involved a relativistic outÑow of pairs and hard gamma rays, plausibly triggered by a large propagating fracture in the crust of a neutron star with a Ðeld exceeding 1014 G. Later stages in the light curve are accurately Ðtted by a model for emission from the envelope of a magnetically conÐned pair-photon Ðreball, anchored to the surface of the rotating star, which contracts as it emits X-rays and then evaporates completely in a Ðnite time. The complex four-peaked shape of the light curve likely provides the most direct evidence known for a multipolar geometry in the magnetic Ðeld of a neutron star.

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Section: Reanalysis Of the Signe And Isee-3 Data On The March 5 Eventmentioning

confidence: 65%

The Giant Flare of 1998 August 27 from SGR 1900+14. I. An Interpretive Study ofBeppoSAXandUlyssesObservations

Feroci

Hurley

Duncan

et al. 2001

ApJ

127

172

View full text Add to dashboard Cite

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“…Although long GRBs are most likely of the cosmological origin, it is possible that short GRBs have another origin (probably, even galactic) and are associated with giant SGR flares [65].…”

Section: Discussionmentioning

confidence: 99%

“…34). The only study devoted to the interpretation of such lines in the cosmological model [40] is based on considering the spectrum strongly shifted in the blue region (the corresponding relativistic factor Γ = 25 − 100) for the The spectrum obtained during the first 8 s with the absorption line at an energy of ≈ 65 keV and a wide emission structure in the region of 350 -650 keV, (4) the spectrum of the fourth 4-s interval, and (68) the total spectrum of the sixth, seventh, and eighth intervals [65]. gas cloud illuminated by the fireball γ rays.…”

Section: Lines In the Hard X-ray Regionmentioning

confidence: 99%

Cosmic γ-ray bursts: Observations and modeling

Бисноватый-Коган

2006

Phys. Part. Nuclei

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It is now commonly accepted that cosmic γ -ray bursts (GRBs) are of cosmological origin. This conclusion is based on the statistical analysis of GRBs and the measurements of line redshifts in GRB optical afterglows, i.e., in the so-called long GRBs. In this review, the models of radiation and models of GRB sources are considered. In most of these models, if not in all of them, the isotropic radiation cannot provide the energy release necessary for the appearance of a cosmological GRB. No correlation is noted between the redshift, the GRB-spectrum shape, and the total detected energy. The comparison between data obtained in the Soviet experiment KONUS and the American experiment BATSE shows that they substantially differ in statistical properties and the detection of hard x-ray lines. The investigation of hard gamma (0.110 GeV) afterglows, the measurement of prompt optical spectra during the GRB detection, and the further investigation of hard x-ray lines is of obvious importance for gaining insight into the GRB origin. Observations of two bright optical GRB afterglows point to the fact that an initially bright optical flare is directly related to the GRB itself, and the subsequent weak and much more continuous optical radiation is of a different nature. The results of observations of optical GRB afterglows are discussed. They point to the fact that the GRBs originate in distant galaxies with a high matter density, where intense star formation takes place. The interaction of the cosmological GRB radiation with a dense surrounding molecular cloud results in the appearance of long-duration (up to 10 years) weak optical afterglows associated with the heating and reradiation of gas. Results of 2D numerical simulation of the heating and reradiation of gas in various variants of the relative disposition of GRB and molecular clouds are presented. In conclusion, the possible relation between

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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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The 5 March 1979 event and the distinct class of short gamma bursts: are they of the same origin?

Cited by 95 publications

References 14 publications

The Giant Flare of 1998 August 27 from SGR 1900+14. I. An Interpretive Study ofBeppoSAXandUlyssesObservations

The Giant Flare of 1998 August 27 from SGR 1900+14. I. An Interpretive Study ofBeppoSAXandUlyssesObservations

Cosmic γ-ray bursts: Observations and modeling

Evolutions of Neutron Stars and their Magnetic Fields

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