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We report observations of white-light ejecta in the low corona, for twoX-class flares on the 2013 May 13, using data from the Helioseismic andMagnetic Imager (HMI) of the Solar Dynamics Observatory. At least two distinctkinds of sources appeared (chromospheric and coronal), in the early and laterphases of flare development, in addition to the white-light footpoint sourcescommonly observed in the lower atmosphere. The gradual emissions have a clearidentification with the classical loop-prominence system, but are brighter thanexpected and possibly seen here in the continuum rather than line emission. Wefind the HMI flux exceeds the radio/X-ray interpolation of the bremsstrahlungproduced in the flare soft X-ray sources by at least one order of magnitude.This implies the participation of cooler sources that can produce free-boundcontinua and possibly line emission detectable by HMI. One of the early sourcesdynamically resembles "coronal rain", appearing at a maximum apparent heightand moving toward the photosphere at an apparent constant projected speed of134 $\pm$ 8 $\mathrm{km s^{-1}}$. Not much literature exists on the detectionof optical continuum sources above the limb of the Sun by non-coronagraphicinstruments, and these observations have potential implications for our basicunderstanding of flare development, since visible observations can in principleprovide high spatial and temporal resolution.

Chromospheric and Coronal Observations of Solar Flares with the Helioseismic and Magnetic Imager