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We report on G-band emission observed by the Solar Optical Telescope onboardthe Hinode satellite in association with the X1.5-class flare on 2006 December14. The G-band enhancements originate from the footpoints of flaring coronalmagnetic loops, coinciding with non-thermal hard X-ray bremsstrahlung sourcesobserved by the Reuven Ramaty High Energy Solar Spectroscopic Imager. At theavailable 2 minute cadence, the G-band and hard X-ray intensities arefurthermore well correlated in time. Assuming that the G-band enhancements arecontinuum emission from a blackbody, we derived the total radiative losses ofthe white-light flare (white-light power). If the G-band enhancementsadditionally have a contribution from lines, the derived values areoverestimates. We compare the white-light power with the power in hard X-rayproducing electrons using the thick target assumption. Independent of thecutoff energy of the accelerated electron spectrum, the white-light power andthe power of accelerated electrons are roughly proportional. Using the observedupper limit of ~30 keV for the cutoff energy, the hard X-ray producingelectrons provide at least a factor of 2 more power than needed to produce thewhite-light emission. For electrons above 40 keV, the powers roughly match forall four of the time intervals available during the impulsive phase. Hence, theflare-accelerated electrons contain enough energy to produce the white-lightflare emissions. The observed correlation in time, space, and power stronglysuggests that electron acceleration and white-light production in solar flaresare closely related. However, the results also call attention to theinconsistency in apparent source heights of the hard X-ray (chromosphere) andwhite-light (upper photosphere) sources.

G-band and Hard X-ray Emissions of the 2006 December 14 flare observed by Hinode/SOT and RHESSI