A modified spectral analysis technique is used to study the temporal structure of the emission from the γ-ray burst GRB 080319B detected in three space missions, Swift/BAT, Wind/KONUS, and Integral/SPI ACS. The energy range of the γ rays detected in these experiments covers 15-10000 keV. The time resolution for the first two of these experiments was 64 ms and for the third, 50 ms. Quasiperiodic oscillations with periods from 0.6 s to 6 s were observed. To within the time resolution, the oscillations with periods of 1.28, 0.89, and 0.64 s are the second, third, and fourth harmonics, respectively, of oscillations with a period of 2.56 s, while oscillations with a period of 0.96 s are the third harmonic of oscillations with a period of 2.94 s. The behavior of the quasiperiodic components is examined as a function of the phase of the events. Possible physical mechanisms for the quasiperiodic oscillations in the light curves of γ-ray bursts are discussed.
The spectral lags of gamma ray bursts are defined as the difference in the registration time of the same radiation pulse in different energy channels of the recording device. This parameter can characterize both the mechanism of radiation generation by the source and the physical conditions of radiation propagation from the source to the observer. In this paper, the dependence of the arrival time of photons on their energy for the gamma ray burst GRB 190114C is obtained from the data of the Gamma ray Burst Monitor (NaI detectors) of the Fermi Gamma ray Space Telescope. It is shown that this dependence is mainly due to the back edges of the light curve pulses. The spectral lags of the leading edges of the pulses are small and comparable in magnitude to the measurement errors. The observed anomaly in the energy range from 5 to 20 keV is probably related to the quasi-thermal radiation of the source.
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