3-10 keV and 0. 1- to 2-MeV observations of four gamma-ray bursts

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Four catalogued ..gamma..-ray bursts that occurred between 79/3/7 and 79/7/31 have been observed over the 3 to 10 keV range by a joint NRL/Los Alamos experiment on the Air Force P78-1 satellite. The bursts were also well observed by members of the interplanetary network. In this paper we present hardness ratios, x-ray/..gamma..-ray luminosity ratios, and time histories. The most significant results presented herein can be summarized as follows: (1) gamma-ray bursters can emit fairly strongly at x-ray energies near the time of the ..gamma.. burst with L/sub x//L/sub ..gamma../ approx. .02 (L/sub x/ approx. 10/sup 37/ ergs s/sup -1/, 3 ... continued below

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Pages: 13

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Laros, J.G.; Evans, W.D.; Fenimore, E.E.; Klebesadel, R.W.; Shulman, S. & Fritz, G. January 1, 1983.

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Four catalogued ..gamma..-ray bursts that occurred between 79/3/7 and 79/7/31 have been observed over the 3 to 10 keV range by a joint NRL/Los Alamos experiment on the Air Force P78-1 satellite. The bursts were also well observed by members of the interplanetary network. In this paper we present hardness ratios, x-ray/..gamma..-ray luminosity ratios, and time histories. The most significant results presented herein can be summarized as follows: (1) gamma-ray bursters can emit fairly strongly at x-ray energies near the time of the ..gamma.. burst with L/sub x//L/sub ..gamma../ approx. .02 (L/sub x/ approx. 10/sup 37/ ergs s/sup -1/, 3 to 10 keV, assuming a distance of 1 kpc); (2) the centroid of the x-ray emission generally lags the ..gamma..-ray centroid, but there is also evidence for one or more types of x-ray precursor activity; (3) the ..gamma..-ray hardness ratios were not highly variable for these particular events. However, there is some evidence that the ..gamma..-ray spectra softened near the ends of the bursts when the x-ray/..gamma..-ray ratios were high; (4) the x-ray/..gamma..-ray power law number index during times of the strongest ..gamma..-ray emission ranged from 0.8 to approx. 1.1 for the four bursts; (5) the x-ray tail of GB790307 probably can be modeled as the cooling of hot plasma generated during the ..gamma..-ray burst. Simple versions of this model can be used to estimate various source parameters. These estimates imply a distance of a few hundred to a few thousand pc; (6) gamma-ray bursters probably do not produce events similar to classical x-ray bursts independently of the ..gamma..-ray emission.

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Pages: 13

Notes

NTIS, PC A02/MF A01.

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  • Workshop on high energy transients, Santa Cruz, CA, USA, 11 Jul 1983

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  • Other: DE84001334
  • Report No.: LA-UR-83-2657
  • Report No.: CONF-830797-5
  • Grant Number: W-7405-ENG-36
  • Office of Scientific & Technical Information Report Number: 5651249
  • Archival Resource Key: ark:/67531/metadc1093572

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  • January 1, 1983

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  • Feb. 10, 2018, 10:06 p.m.

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  • March 20, 2018, 5:17 p.m.

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Laros, J.G.; Evans, W.D.; Fenimore, E.E.; Klebesadel, R.W.; Shulman, S. & Fritz, G. 3-10 keV and 0. 1- to 2-MeV observations of four gamma-ray bursts, article, January 1, 1983; United States. (digital.library.unt.edu/ark:/67531/metadc1093572/: accessed July 19, 2018), University of North Texas Libraries, Digital Library, digital.library.unt.edu; crediting UNT Libraries Government Documents Department.