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White-light emissions were observed from an X1.7 class solar flare on 27January 2012, using three continuum bands (red, green, and blue) of the SolarOptical Telescope (SOT) onboard the Hinode satellite. This event occurred nearthe solar limb, and so differences in locations of the various emissions areconsistent with differences in heights above the photosphere of the variousemission sources. Under this interpretation, our observations are consistentwith the white-light emissions occurring at the lowest levels of where the CaII H emission occurs. Moreover, the centers of the source regions of the red,green, and blue wavelengths of the white-light emissions are significantlydisplaced from each other, suggesting that those respective emissions areemanating from progressively lower heights in the solar atmosphere. Thetemperature distribution was also calculated from the white-light data, and wefound the lower-layer emission to have a higher temperature. This indicatesthat high-energy particles penetrated down to near the photosphere, anddeposited heat into the ambient lower layers of the atmosphere.

Emission Height and Temperature Distribution of White-Light Emission Observed by Hinode/SOT from the 2012 January 27 X-class Solar Flare