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Дата изменения: Thu Dec 17 16:19:14 2015
Дата индексирования: Sun Apr 10 00:18:26 2016
Кодировка: koi8-r
Поисковые слова: m8
GCN Circ.: 5173, 5177, 5183, 5186, 5189, 5193
The afterglow light curve was measured in detail starting from about 5 h
after the GRB and over five ensuing nights. In addition, upper limits were
obtained on the rapid variability of the afterglow on the first night of
observations and the history of afterglow color variations was measured in
detail. In the time interval from 6 to 16h after the burst, the flux
gradually decreased approximately as a power law with a slope of
-1.14+-0.02. After that, variability was observed on a time scale δt <
t and the afterglow started to decay faster. The afterglow color was
approximately constant (V-R ≈ 0.5) throughout the observations,
despite the flux variability. Variability time scales up to δt ≈
0.0055 were observed at ΔFν/Fν ≈ 0.3, which violates
constraints on the variability of the observed emission from an
ultrarelativistic jet obtained by Ioka et al. (2005) for simle models. We
suggest to explain this variability by the fact that the shell motion is no
longer ultrarelativistic at this time.
