000004549 001__ 4549
000004549 005__ 20200115144924.0
000004549 037__ $$aCTALK-2020-0027
000004549 100__ $$aMagdalenic, Jasmina
000004549 245__ $$aActive region jets on August 25, 2011   
000004549 260__ $$c2019
000004549 269__ $$c2019-05-06
000004549 520__ $$aSolar coronal jets are impulsive, collimated features, observed at different energies. Jets are seen on the Sun at all scales - from those occurring in coronal holes to those in active regions.  The process of creating jets is mostly considered to be related to reconnection between open and closed field lines. This study is focused on the active region jets which occur regularly at small-scale, but can also occur on a larger scale related to CMEs and SEPs. The aim of the study is to determine why the jets occurred in this particular active region, what their dynamics are, and possibly to predict what we might see with Solar Orbiter. Understanding the process of  jets  requires  spectral  and  imaging  data  across  different  energy  regimes.  Therefore,  we selected well observed series of jets which occurred on August 25, 2011, in the active region  NOAA 1271 (located near the western solar limb). First results of the multiwavelength study show that the repeated jets observed on August 25, originate from the western part of the active region and were associated with a small flux emergence. Due to the existence of open field lines but also a large trans-equatorial loop system (closed field lines), some of the type III radio bursts associated with jets propagated to the interplanetary space and some did not. In the  first  radio  triangulation  study  of  radio  emission  associated  with  jets,  we  employed goniopolarimetric measurements taken simultaneously from STEREO A and WIND spacecraft.  The reconstructed propagation paths of the interplanetary type III bursts associated with jets indicate that the fast electron beams are propagating towards the Earth, but the path does not completely coincide with the Parker spiral. This deviation in the propagation path of the electron beams associated with jets is probably due to the influence of a nearby coronal hole.
000004549 594__ $$aNO
000004549 700__ $$aJebaraj, Immanuel
000004549 700__ $$aHarra, Louis
000004549 700__ $$aMatthews, S
000004549 700__ $$aBerghmans, David
000004549 700__ $$aKrupar, Vratislav
000004549 773__ $$tCESRA 2019, Potsdam
000004549 8560_ $$fimmanuel.jebaraj@observatoire.be
000004549 906__ $$aInvited
000004549 980__ $$aCTALKINVI