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Coronal mass ejections (CMEs) are often accompanied by coronal dimmingevident in extreme ultraviolet (EUV) and soft X-ray observations. The locationsof dimming are sometimes considered to map footpoints of the erupting fluxrope. As the emitting material expands in the corona, the decreased plasmadensity leads to reduced emission observed in spectral and irradiancemeasurements. Therefore, signatures of dimming may reflect properties of CMEsin the early phase of its eruption. In this study, we analyze the event offlare, CME, and coronal dimming on December 26, 2011. We use the data from theAtmospheric Imaging Assembly (AIA) on Solar Dynamics Observatories (SDO) fordisk observations of the dimming, and analyze images taken by EUVI, COR1, andCOR2 onboard the Solar Terrestrial Relations Observatories to obtain the heightand velocity of the associated CMEs observed at the limb. We also measuremagnetic reconnection rate from flare observations. Dimming occurs in a fewlocations next to the flare ribbons, and it is observed in multiple EUVpassbands. Rapid dimming starts after the onset of fast reconnection and CMEacceleration, and its evolution well tracks the CME height and flarereconnection. The spatial distribution of dimming exhibits cores of deepdimming with a rapid growth, and their light curves are approximately linearlyscaled with the CME height profile. From the dimming analysis, we infer theprocess of the CME expansion, and estimate properties of the CME.

The Nature of CME-Flare Associated Coronal Dimming