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Total solar eclipse (TSE) coronal large and small scale events were reportedin the historical literature but a definite synoptic coverage was missing forstudying a relationship with the more general magnetic context of thesolar-disk. We here analyze temporal changes in the solar corona before,during, and after the total solar eclipse on 21 August 2017 from a set ofground-based and of space-borne observations. High-quality ground-basedwhite-light (W-L) observations and a deep image processing allow us to revealthese changes for the first time with a fraction of a one-minute timeresolution. Displacements of a number of fine coronal features were measuredfor the first time at these small radial distances, using a diffraction limitedinstrument at a single site. The comparison with space-based observations,including observations from the {\it Solar Terrestrial Relations Observatory}(STEREO) mission, showed that the features belong to a slow coronal massejection (CME) propagating through the corona with the nearly constant speed of250 km/s. Our TSE images provide the same typical velocity as measured at adistance of one solar radius from the surface. The event was initiated bycoronal dynamics manifested by a prominence eruption that started just beforethe eclipse observations and an ascent of a U-shaped structure visible in theAIA 171 A channel, which we assume as the lower part of a coronal cavity. Theprominence material was observed draining down towards the chromosphere alongthe prominence arch. While the prominence disappears in the STEREO-Afield-of-view at the height of about 6$^{\prime}$ above the limb, thecorresponding flux rope seems to continue towards the outer corona and producesthe slow CME with turbulent motion. The overall mass of the moving features isevaluated based on absolute photometrical data extracted from our best W-Leclipse image.

Solar Total Eclipse of 21 August 2017: Study of the Inner Corona Dynamical Events Leading to a CME