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Coronal dimming of extreme ultraviolet (EUV) emission has the potential to bea useful forecaster of coronal mass ejections (CMEs). As emitting materialleaves the corona, a temporary void is left behind which can be observed inspectral images and irradiance measurements. The velocity and mass of the CMEsshould impact the character of those observations. However, other physicalprocesses can confuse the observations. We describe these processes and theexpected observational signature, with special emphasis placed on thedifferences. We then apply this understanding to a coronal dimming event withan associated CME that occurred on 2010 August 7. Data from the Solar DynamicsObservatory's (SDO) Atmospheric Imaging Assembly (AIA) and EUV VariabilityExperiment (EVE) are used for observations of the dimming, while the Solar andHeliospheric Observatory's (SOHO) Large Angle and Spectrometric Coronagraph(LASCO) and the Solar Terrestrial Relations Observatory's (STEREO) COR1 andCOR2 are used to obtain velocity and mass estimates for the associated CME. Wedevelop a technique for mitigating temperature effects in coronal dimming fromfull-disk irradiance measurements taken by EVE. We find that for this event,nearly 100% of the dimming is due to mass loss in the corona.

Mechanisms and Observations of Coronal Dimming for the 2010 August 7 Event