Statistics of Coronal Dimmings Associated with Coronal Mass Ejections. II. Relationship between Coronal Dimmings and Their Associated CMEs

K. Dissauer, A. M. Veronig, M. Temmer, T. Podladchikova

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    34 Citations (Scopus)


    We present a statistical study of 62 coronal dimming events associated with Earth-directed coronal mass ejections (CMEs) during the quasi-quadrature period of STEREO and the Solar Dynamics Observatory (SDO). This unique setting allows us to study both phenomena in great detail and compare characteristic quantities statistically. Coronal dimmings are observed on-disk by the SDO/Atmospheric Imaging Assembly and the Helioseismic and Magnetic Imager, while the CME kinematics during the impulsive acceleration phase is studied close to the limb with STEREO/EUVI and COR, minimizing projection effects. The dimming area, its total unsigned magnetic flux, and its total brightness, reflecting properties of the total dimming region at its final extent, show the highest correlations with the CME mass (c ∼ 0.6-0.7). Their corresponding time derivatives, describing the dynamics of the dimming evolution, show the strongest correlations with the CME peak velocity (c ∼ 0.6). The highest correlation of c = 0.68 ±0.08 is found with the mean intensity of dimmings, indicating that the lower the CME starts in the corona, the faster it propagates. No significant correlation between dimming parameters and the CME acceleration was found. However, for events where high-cadence STEREO observations were available, the mean unsigned magnetic field density in the dimming regions tends to be positively correlated with the CME peak acceleration (c = 0.42 ±0.20). This suggests that stronger magnetic fields result in higher Lorentz forces providing stronger driving force for the CME acceleration. Specific coronal dimming parameters correlate with both CME and flare quantities providing further evidence for the flare-CME feedback relationship. For events in which the CME occurs together with a flare, coronal dimmings statistically reflect the properties of both phenomena.

    Original languageEnglish
    Article number123
    JournalAstrophysical Journal
    Issue number2
    Publication statusPublished - 1 Apr 2019


    • Sun: activity
    • Sun: corona
    • Sun: coronal mass ejections (CMEs)
    • Sun: flares


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