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Multiwavelength observations of the Soft Gamma-Ray Repeaters
AIP Conference Proceedings, 1996We present the current status of the multiwavelength observations of the quiescent counterparts to the Soft Gamma‐Ray Repeaters, and out‐line our future observing plans. The preliminary observations suggest that the plerion model is not appropriate for these sources.
Smith, I.A. +13 more
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Models of Soft Gamma-Ray Repeater Emissions
Astrophysics and Space Science, 1995We review emission models of soft gamma-ray repeaters (SGRs) within the context of magnetized neutron star origins. Motivations for moderate field (≤1010–12G) versus ultrastrong field (≥ 5 × 1014G) neutron stars are considered. Implications for the astrophyiscal models are discussed.
Edison P Liang
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Soft gamma-ray repeater spectral properties
AIP Conference Proceedings, 1996If typical GRBs have X‐ray counterparts similar to those detected by GINGA, then existing focussing X‐ray telescopes will be able to detect GRBs three orders of magnitude fainter than the detection limit of BATSE. The EINSTEIN Observatory observed nearby galaxies for approximately 2 million seconds, during which time only one burstlike X‐ray transient ...
C. Kouveliotou +5 more
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Recent observations of Soft Gamma-ray Repeaters
AIP Conference Proceedings, 2008Soft Gamma‐ray Repeaters (SGRs) were the first objects interpreted as magnetars: isolated neutron stars powered by the decay of extremely high magnetic fields. I review the results obtained in the last few years with X‐ray and γ‐ray observations of the four confirmed SGRs.
Sandro Mereghetti +3 more
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AIP Conference Proceedings, 1997
The Soft Gamma-Ray Repeaters (SGR) are sources of brief intense outbursts of low energy gamma rays. Most likely they are a new manifestation of neutron stars. Three sources were known prior to the launch of CGRO, and bursts from two of these have been seen by BATSE.
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The Soft Gamma-Ray Repeaters (SGR) are sources of brief intense outbursts of low energy gamma rays. Most likely they are a new manifestation of neutron stars. Three sources were known prior to the launch of CGRO, and bursts from two of these have been seen by BATSE.
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The identification of a supernova remnant with a soft gamma ray repeater
AIP Conference Proceedings, 1994Earlier we had shown that the well‐located SGR 1806−20 was coincident with the radio supernova remnant G 10.0–0.3, with a low chance probability. Recent high energy observations have left little doubt as to the veracity of this association. We present new radio observations of G 10.0–0.3 revealing a hierarchy of nested, amorphous regions, in which a ...
D. A. Frail, S. R. Kulkarni
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Millimeter observations of the soft gamma-ray repeater SGR1806−20
AIP Conference Proceedings, 1996We observed in 1994 and 1995 the Soft Gamma‐Ray Repeater SGR1806−20 in the CO(J=1−0), 13CO(J=1−0), CO(J=2−1), HCN(J=1−0), HCN(J=2−1), CN(J=1−0), CN(J=2−1) lines, using the SEST millimeter radio telescope. We were attempting to estimate the distance of SGR1806−20 as well as to demonstrate the association of a molecular cloud with the optical/X‐ray ...
Ph. Durouchoux +3 more
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Infrared observations of soft gamma-ray repeaters
Fourth Huntsville gamma-ray burst symposium, 1998Quiescent stellar counterparts have been suggested for the Soft Gamma-Ray Repeaters SGR 1806−20 and SGR 1900+14, while none have been found for SGR 0525−66. This paper gives a brief overview of some recent and ongoing infrared observing programs. For a more detailed review article, see Smith [2].
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Universal statistics of soft gamma-ray repeating (SGR) bursts
Physics of Particles and Nuclei, 2018Soft gamma repeater (SGR) bursts are considered as a release of magnetic energy stored in the baryon degrees of freedom of the magnetar crust. It is shown that this interpretation allows all observations of these bursts to be systematized and universal statistical properties to be revealed and explained.
V. N. Kondratyev, Yu. V. Korovina
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A luminous companion to the soft gamma-ray repeater 1806−20
AIP Conference Proceedings, 1996The association of the soft γ‐ray repeater SGR 1806−20 with a plerion has led to the hypothesis that SGRs are young pulsars. However, it remains a mystery why only some pulsars become SGRs, and how a pulsar can produce the observed brilliant bursts of γ rays. Models involving a companion could address both issues.
M. H. van Kerkwijk, S. R. Kulkarni
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