Orateur
Summary
In this talk, I will briefly overview the synchrotron X-ray variability of TeV
blazars by focusing how to extract "jet physics" from the observed light
curves. Apparently, the light curve gives independent and complementary
information to the spectral energy distribution, but surprisingly
little attention
has been paid especially for the blazar study. Various temporal techniques
are given in literature, e.g., the discrete correlation function (DCF), the
structure function (SF), and the power spectrum density (PSD) analysis,
but special care must be taken if the data is not well sampled and relatively
short compared to the variability time-scale of the system. For example, there
was a beautiful paradigm that the soft X-ray variation of TeV blazars
lag behind
the hard X-rays by ~5 ksec, reflecting the difference of synchrotron cooling
time-scale. However, the situation is being more and more complicated if we
properly consider the effects caused by periodic gap in the light curve due
to the Earth occultation (every ~ 6ksec). I will present detailed simulations
to see how the "gap" and the "length" of the data affects the results
of temporal
analysis, and to what extent we can be sure of our results. I will also briefly
present some recent highlights from Suzaku observations of TeV blazars.
