000004010 001__ 4010
000004010 005__ 20190130230156.0
000004010 037__ $$aCTALK-2019-0068
000004010 100__ $$aSarkar, Ranadeep
000004010 245__ $$aSH33H-3727: Evolution of Coronal Cavity from Quiescent to Eruptive Phase in Association with Coronal Mass Ejection
000004010 260__ $$c2018
000004010 269__ $$c2018-12-12
000004010 520__ $$aThe initiation mechanism of coronal mass ejections (CMEs) remains among the most elusive topics in solar physics. The initiation and triggering of CMEs can be studied by observing the coronal cavities in the lower coronal regions. These cavities appear as dark features and are believed to be the density depleted cross-sections of the magnetic flux ropes, where the magnetic field strength attains a much higher value compared to the background corona. Cavities may last for days or even weeks and evolve as the dark core part of the CME during the eruptive phase. In order to understand the pre-eruptive stability conditions for quiescent cavities and the triggering mechanisms for those structures to erupt, it is important to study the morphological evolution of the coronal cavities. In this work, we study the evolution of a cavity in lower corona using the observations from STEREO SECCHI/EUVI and PROBA2/SWAP EUV imager. In the quiescent phase, the cavity centroid height slowly rises from 1.10 to 1.23 RS during its passage on the visible solar disc from May 30 to June 13, 2010 and its initial circular shaped morphology gradually expanded and evolved into elliptical shape prior to the eruption from the western solar limb. The extended field-of-view of SWAP fills the observational gap between 1 to 2 RS . It enables us to capture the complete evolution of the erupting cavity starting from its EUV counterpart in the lower corona up to the white light cavity morphology seen in LASCO C2/C3 field-of-view. During the eruptive phase, we have observed a significant non-radial motion of the cavity at a very low coronal height of 1.3 RS . Furthermore, the geometrical fitting to the cavity morphology in different time-steps during its eruptive phase reveals that it exhibits non-self similar expansion in the lower corona. We also discuss the role of the background magnetic field and the possible instabilities which may lead to the non-radial motion and initiation of the cavity eruption respectively.
000004010 536__ $$a3ESA-PROBA2SOC/$$c3ESA-PROBA2SOC/$$f3ESA-PROBA2SOC
000004010 594__ $$aNO
000004010 700__ $$aSrivastava , Nandita
000004010 700__ $$aMierla, Marilena
000004010 700__ $$aWest, Matthew
000004010 700__ $$aD'Huys, Elke
000004010 773__ $$tAGU Washington DC
000004010 8560_ $$fmatthew.west@observatoire.be
000004010 85642 $$ahttps://agu.confex.com/agu/fm18/meetingapp.cgi/Paper/410847
000004010 906__ $$aContributed
000004010 980__ $$aCTALKCONT