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Title:
BATSE observations of gamma-ray burst spectra. 2: Peak energy evolution in bright, long bursts
Authors:
Ford, L. A.; Band, D. L.; Matteson, J. L.; Briggs, M. S.; Pendleton, G. N.; Preece, R. D.; Paciesas, W. S.; Teegarden, B. J.; Palmer, D. M.; Schaefer, B. E.; Cline, T. L.; Fishman, G. J.; Kouveliotou, C.; Meegan, C. A.; Wilson, R. B.; Lestrade, J. P.
Affiliation:
AA(University of California at San Diego, La Jolla, CA), AB(University of California at San Diego, La Jolla, CA), AC(University of California at San Diego, La Jolla, CA), AD(University of Alabama at Huntsville, Huntsville, AL), AE(University of Alabama at Huntsville, Huntsville, AL), AF(University of Alabama at Huntsville, Huntsville, AL), AG(University of Alabama at Huntsville, Huntsville, AL), AH(NASA/Goddard Space Flight Center, Greenbelt, MD), AI(NASA/Goddard Space Flight Center, Greenbelt, MD), AJ(NASA/Goddard Space Flight Center, Greenbelt, MD), AK(NASA/Goddard Space Flight Center, Greenbelt, MD), AL(NASA/Marshall Space Flight Center, Huntsville, AL), AM(NASA/Marshall Space Flight Center, Huntsville, AL), AN(NASA/Marshall Space Flight Center, Huntsville, AL), AO(NASA/Marshall Space Flight Center, Huntsville, AL), AP(Mississippi State University, Mississippi State, MS)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 439, no. 1, p. 307-321 (ApJ Homepage)
Publication Date:
01/1995
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
Gamma Ray Bursts, Gamma Ray Spectra, Radiant Flux Density, Spectral Energy Distribution, Astronomical Models, Gamma Ray Observatory, Spectrum Analysis, Statistical Analysis
DOI:
10.1086/175174
Bibliographic Code:
1995ApJ...439..307F

Abstract

We investigate spectral evolution in 37 bright, long gamma-ray bursts observed with the Burst and Transient Source Experiment (BATSE) spectroscopy detectors. High-resolution spectra are chracterized by the energy of the peak of nu Fnu, and the evolution of this quantity is examined relative to the emission intensity. In most cases it is found that this peak energy either rises with or slightly precedes major intensity increases and softens for the remainder of the pulse. Interpulse emission is generally harder early in the burst. For bursts with multiple intensity pulses, later spikes tend to be softer than earlier ones, indicating that the energy of the peak of nu Fnu is bounded by an envelope which decays with time. Evidence is found that bursts in which the bulk of the flux comes well after the event which triggers the instrument tend to show less peak energy variability and are not as hard as several bursts in which the emission occurs promptly after the trigger. Several recently proposed burst models are examined in light of these results and no qualitative conflicts with the observations presented here are found.

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