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The Solar Optical Telescope (SOT) on board Hinode satellite observed an X3.4class flare on 2006 December 13. Typical two-ribbon structure was observed, notonly in the chromospheric CaII H line but also in G-band and FeI 6302A line.The high-resolution, seeing-free images achieved by SOT revealed, for the firsttime, the sub-arcsec fine structures of the "white light" flare. The G-bandflare ribbons on sunspot umbrae showed a sharp leading edge followed by adiffuse inside, as well as previously known core-halo structure. The underlyingstructures such as umbral dots, penumbral filaments and granules were visiblein the flare ribbons. Assuming that the sharp leading edge was directly heatedby particle beam and the diffuse parts were heated by radiative back-warming,we estimate the depth of the diffuse flare emission using the intensity profileof the flare ribbon. We found that the depth of the diffuse emission is about100 km or less from the height of the source of radiative back-warming. Theflare ribbons were also visible in the Stokes-V images of FeI 6302A, as atransient polarity reversal. This is probably related to "magnetic transient"reported in the literature. The intensity increase in Stokes-I images indicatesthat the FeI 6302A line was significantly deformed by the flare, which maycause such a magnetic transient.

Flare Ribbons Observed with G-band and FeI 6302A Filters of the Solar Optical Telescope on Board Hinode