Atsunori Yonehara
, PASA, 18 (2), in press.
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Introduction
Since the discovery of quasars, one of the attractive subjects in astronomy/astrophysics is to reveal their structure. Currently, previous observational and theoretical studies strongly suggest the existence of an accretion disk in the innermost region of quasars. The apparent size of the accretion disk is estimated to be 
. Unfortunately, due to such small apparent angular size, it is impossible to resolve the accretion disk directly. Thus, we do not have any direct evidence for the existence of the accretion disk. However, there is a fascinating way to get rid of such difficulties; the diagnosis method by using ``quasar microlensing''. Applicable targets for such a technique are limited (e.g., Q2237+0305), but surprisingly, the spatial resolution of the technique (
) reaches far below that of current observational instruments. Thus, we can probe the innermost region of quasars via microlensing (e.g., see Wambsganss 2001 and Mineshige et al. 2001 in this volume). Recently, the OGLE group has reported evident signals of quasar microlensing in Q2237+0305 (so-called ``Huchra's lens'' or ``Einstein Cross'', see Wozniak et al. 2000). Here, I present an analysis of the quasar microlensing light curve of image C (see also Shalyapin 2001). In section 2, I briefly explain the method of light-curve fitting, and the results and discussions are presented in section 3.
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