Titlebook: Gamma-Ray Bursts in the Afterglow Era; Proceedings of the I Enrico Costa,Filippo Frontera,Jens Hjorth Conference proceedings 2001 Springer-

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Estimation of Emission Time Parameter for APEX Experiment,ime are estimated for 49 long APEX bursts detected with time resolution of 0.125 sec and 16 short event detected by time-to-spill mode with time resolution of fraction of ms. The APEX data is shown to confirm the bi-modaldistribution of emission time values found for BATSE bursts.

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Angewandte Mathematik: Body and Souler the past severaly ears. The emphasis is on a) the more surprising or unusualresul ts which have not been discussed in the BATSE review talk at this meeting, and b) the energy range above about 25 keV.

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Angewandte Mathematik: Body and Souls itself as a strong correlation between instantaneous energy flux . and peak energy ... In the (.,..) plane, the correlation produces distinct tracks in the form of branches and loops representing the different parts of a burst time history. Despite the variety of features seen in different events,

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Grundlegende Matrizenoperationen, but remaining undetected in the Gamma Ray Bursts Monitor on BeppoSAX. They have properties very similar to the x-ray counterparts of GRBs and account for some of the Fast X-ray Transient events seen in almost every x-ray satellite. We review their X-ray properties and show that x-ray flashes are in

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https://doi.org/10.1007/978-3-662-05743-8and the ProportionalCoun ter Array (PCA) instruments have detected 30 GRBs. In 16 cases, an early celestial position was released to the community, sometimes in conjunction with IPN results. The subsequent optical and radio searches led to the detection of 5 x-ray afterglows, to at least 6 optical o

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Besonderheiten der bodennahen Turbulenz,poSAX data. This model gives a satisfactory description of the majority of the data. Nevertheless, . 30% need of accounting for substantial radiative cooling of the emitting electrons during the event.

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K. Friehs,B. Hitzmann,T. Scheperell as the number of distinct pulse structures per burst. Performing the cross-correlation between two energy bands, we measure an average lag .-40 x shorter than for long bursts, and a lag distribution close to symmetric about zero - unlike long bursts. Using a “Bayesian Block” method to identify s

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Soziale Wohlfahrt und Sozialwahltheorie,is operating since April, 2000. When a true celestial burst is recognized, this S/W yields some relevant data, like peak counts, total counts, duration. In the near future, the possible incoming direction will be included as well. This info is promptly and automatically distributed, in a fixed forma