000003471 001__ 3471
000003471 005__ 20180129172124.0
000003471 037__ $$aCTALK-2018-0047
000003471 100__ $$aWest, Matthew
000003471 245__ $$aPost-Flare Giant Arches - Unanswered Questions
000003471 260__ $$c2017
000003471 269__ $$c2017-12-15
000003471 520__ $$aRecent observations from the SWAP EUV imager on-board PROBA2 and SXI X-ray observations from the GOES satellite have shown that post-flare giant arches and regular post-flare loops are one and the same thing. However, it is still not clear how certain loop systems are able to sustain prolonged growth to heights greater than half a solar-radii. In this presentation we further explore the energy deposition rate above post-flare loop systems through high-energy RHESSI observations. We also explore the difference between the growth of different loop systems through an epoch analysis. The epoch analysis is initially performed over the period when the STEREO satellites were in quadrature with PROBA2 allowing us to assess the difference between their on-disk and on-limb signatures. Giant arches are generally characterised by their height of growth when observed close to the solar limb, but due to the optically thin nature of the EUV solar atmosphere, projection effects and the scarcity of events occurring within 5 degrees of the limb it is not understood how common these events are. Using the analysis during the quadrature period we gain a better understanding of how rare these events are, and by determining characteristic on disk signatures we can combine our data set with magnetogram observations to better understand their magnetic evolution.
000003471 594__ $$aNO
000003471 700__ $$aSeaton, Daniel
000003471 700__ $$aDennis, Brian
000003471 700__ $$aFeng, Li
000003471 700__ $$aPalmerio, Erika
000003471 700__ $$aSavage, Sabrina
000003471 773__ $$tAGU, New Orleans, USA
000003471 8560_ $$fmatthew.west@observatoire.be
000003471 85642 $$ahttps://agu.confex.com/agu/fm17/meetingapp.cgi/Paper/271427
000003471 906__ $$aContributed
000003471 980__ $$aCTALKCONT