000006325 001__ 6325
000006325 005__ 20230201162443.0
000006325 037__ $$aCTALK-2023-0059
000006325 100__ $$aBemporad, A.
000006325 245__ $$aA Coronal Mass Ejection followed by a prominence eruption and a plasma blob as observed by Solar Orbiter
000006325 260__ $$c2022
000006325 269__ $$c2022-09-12
000006325 520__ $$aOn February 12, 2021 two subsequent eruptions occurred above the West limb, as seen along the Sun-Earth line. The first event was a typical slow Coronal Mass Ejection (CME), followed ∼7 hours later by a smaller and collimated prominence eruption, originating Southward with respect to the CME, followed by a plasma blob. These events were observed not only by SOHO and STEREO-A missions, but also by the suite of remote sensing instruments on-board Solar Orbiter (SolO). This work shows how data acquired by the Full Sun Imager (FSI), Metis coronagraph, and Heliospheric Imager (SoloHI) from the SolO perspective can be combined to study the eruptions and the different source regions. Moreover, we show how Metis data can be analyzed to provide new information about solar eruptions. Different 3D reconstruction methods were applied to the data acquired by different spacecraft including remote sensing instruments on-board SolO. Images acquired by both Metis channels in the Visible Light (VL) and H i Ly-α line (UV) were combined to derive physical information on the expanding plasma. The polarization ratio technique was also applied for the first time to the Metis images acquired in the VL channel. The two eruptions were followed in 3D from their source region to their expansion in the intermediate corona. Thanks to the combination of VL and UV Metis data, the formation of a post-CME Current Sheet (CS) was followed for the first time in the intermediate corona. The plasma temperature gradient across a post-CME blob propagating along the CS was also measured for the first time. Application of the polarization ratio technique to Metis data shows that, thanks to the combination of four different polarization measurements, the errors are reduced by ∼5−7%, thus better constraining the 3D distribution of plasma.
000006325 594__ $$aSTCE
000006325 6531_ $$aSolar Orbiter
000006325 6531_ $$aEUI
000006325 700__ $$aManyOtherAuthors, X.
000006325 700__ $$aBerghmans, D.
000006325 700__ $$aD'Huys, E.
000006325 700__ $$aZhukov, A. N.
000006325 773__ $$tSolar Orbiter 8, Belfast (UK)
000006325 8560_ $$fdavid.berghmans@observatoire.be
000006325 85642 $$ahttps://blogs.qub.ac.uk/so8belfast/programme/
000006325 906__ $$aContributed
000006325 980__ $$aCTALKCONT