000008217 001__ 8217
000008217 005__ 20261110112237.0
000008217 037__ $$aCTALK-2026-0155
000008217 100__ $$aBerghmans, D.
000008217 245__ $$aCROSS-SCALE OBSERVATIONS OF SOLAR FLARES BY EUI AND STIX ON SOLAR ORBITER
000008217 260__ $$c2026
000008217 269__ $$c2026-11-03
000008217 520__ $$aMajor solar flares are at the origin of many space weather phenomena.  Besides the flash across the entire spectrum, flares are associated with shock waves, particle acceleration, radio bursts, prominence eruptions and CMEs. Since 2024,  Solar Orbiter has embarked on a series of campaigns to observe Major Solar Flares. In this presentation we discuss the results so far of a series of unique data sets collected mainly by the STIX instrument and the HRIEUV telescope of the EUI instrument.  As an X-ray imaging spectrometer, STIX has continuously  observed on the order of 10^5 flares from solar minimum in 2020 till now.  For the high resolution HRIEUV imager it is much harder to catch a flare, because it can operate only occasionally and with subfield as small as 1/30th of the solar disk at perihelion. Thanks to the so-called short exposures at 2s cadence, HRIEUV can however for the first time observe   flare dynamics at small length & time-scales that have remained veiled for earlier EUV imagers due to pixel saturation & blooming. These Solar Orbiter Major Flare observations indicate that flares are not always the monolithic, catastrophic collapse of an entire magnetic structure but rather a build-up or an  avalanche of magnetic threads reconnecting.  The footpoint kernels in the flare ribbons have time and length-scales that are barely resolved with the 2s cadence /100 km pixel size characteristics of HRIEUV datasets. Also the  width of some post-flare loops are at the 2-pixel scale suggesting the actual width is smaller than 200km. These small scales pose new questions on the required energy and plasma densities.   Whereas the impact of solar flares can be felt at heliospheric scales,  the  data from  Solar Orbiter are thus telling us that the physics driving  major flares, operates at remarkably small spatial and temporal scales. Using this insight for timely flare reporting suggests that modest resolution requirements for monitoring instruments might be suboptimal. 
000008217 594__ $$aSTCE
000008217 6531_ $$aEUI
000008217 6531_ $$asolar flares
000008217 6531_ $$acorona
000008217 700__ $$aChitta,  L.P.
000008217 700__ $$aCollier, H.
000008217 700__ $$aDominique, M. 
000008217 700__ $$aHayes, L.
000008217 700__ $$aKasporova, J.
000008217 700__ $$aKraaikamp , E. 
000008217 700__ $$aLorincik, J.
000008217 700__ $$aRodriguez, L.
000008217 700__ $$aVerbeeck, C. 
000008217 773__ $$tEuropean Space Weather Week 2026, Florence, Italy 
000008217 8560_ $$fdavid.berghmans@ksb-orb.be
000008217 85642 $$ahttps://esww.aeronomie.be/conference/program
000008217 8564_ $$s4899760$$uhttps://publi2-as.oma.be/record/8217/files/20261103-CrossScaleObservationsOfSolarFlares-DavidBerghmans.pdf
000008217 8564_ $$s10738$$uhttps://publi2-as.oma.be/record/8217/files/20261103-CrossScaleObservationsOfSolarFlares-DavidBerghmans.jpg?subformat=icon-180$$xicon-180
000008217 8564_ $$s14615$$uhttps://publi2-as.oma.be/record/8217/files/20261103-CrossScaleObservationsOfSolarFlares-DavidBerghmans.gif?subformat=icon$$xicon
000008217 906__ $$aInvited
000008217 980__ $$aCTALKINVI