In this study we investigate the relationship between RHESSI flares and white light emission as observed by Hinode/SOT at 3968.6 angstroms (Ca II H line), 4306.4 angstroms (G band), and 4505.1 angstroms(blue continuum) images. The emission mechanism for white light emission in flares is not yet understood though it is believed that emission at these wavelengths originates from the chromosphere, photosphere, and deep photosphere respectively. Using a combination of the official RHESSI flare list and a microflare-finding algorithm, we investigate all RHESSI flares with simultaneous observations by RHESSI and Hinode/SOT (a total of ~200 events). Single event studies suggest that microflares are frequently observed in Ca II H line. Photospheric emission is searched for using the location of the Ca II H line chromospheric emission. We discuss the physical conditions necessary that may affect the relationship between HXR and white light emission.