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Blazars show rapid and violent variabilities, which timescale are often less than a day. We studied intraday variations by applying a shot analysis technique to Kepler monitoring of blazar W2R 1926+42 in Quarter 14. We obtained a mean profile calculated from 195 rapid variations. The mean profile shows three components; one is a sharp structure distributed within $pm$0.1 day of the peak, and two slow-varying components. This spiky-peak component reflects features of rapid variations directly. The profile of peak component shows an exponential rise and decay of which timescales are different, 0.0416 and 0.0588 day respectively. This component is too sharp to represent a standard function which is often used to express blazar variations. This asymmetric profile at the peak is difficult to be explained by a simple variation of the Doppler factor by changing a geometry of the emitting region. This result indicates that intraday variations arise from a production of high-energy accelerated particles in the jet.
We analyze the ${it Kepler}$ monitoring light curve of a blazar W2R 1926$+$42 to examine features of microvariability by means of the shot analysis technique. We select 195 intra-day, flare-like variations (shots) for the continuous light curve of Qu
Recently the number of main-sequence and subgiant stars exhibiting solar-like oscillations that are resolved into individual mode frequencies has increased dramatically. While only a few such data sets were available for detailed modeling just a deca
Probing the high energy emission processes of blazars through their variability relies crucially on long-term monitoring. We present unprecedented light curves from unbiased observations of very high energy fluxes from the blazars Mrk 421 and Mrk 501
We report the first results of a systematic investigation to characterize blazar variability power spectral densities (PSDs) at optical frequencies using densely sampled (5--15 minutes integration time), high photometric accuracy ($lesssim$0.2--0.5%)
The typical blazar S5 0716$+$714 is very interesting due to its rapid and large amplitude variability and high duty cycle of micro-variability in optical band. We analyze the observations in I, R and V bands obtained with the $1.0m$ telescope at Weih