000006487 001__ 6487
000006487 005__ 20230817162844.0
000006487 037__ $$aCTALK-2023-0116
000006487 100__ $$aPodladchikova, O.
000006487 245__ $$aPicoflares in the Quiet Solar Corona
000006487 260__ $$c2023
000006487 269__ $$c2023-05-10
000006487 520__ $$aOn May 30, 2020, the Solar Orbiter High-Resolution Imager operating in 174 A being for the first time approximately at a half AU to the Sun, registered a large number of short, small-scale heating events, often called campfires, with rich morphology and smaller space-time characteristics than nanoflares. We estimate the thermal energy of the heating events from increases in the emission measure and temperature using methods assessing thermal energy in flares. We compare these with the characteristics of X-ray flares, in particular, those recorded by the X-ray spectrometer/telescope onboard Solar Orbiter. We found campfires emit thermal energy in picoflares range. The additional previously unaccounted energy input of is about 1% to the total required to sustain quiet solar corona power. The observed frequency distribution would have to continue to the femtoflares range to fulfill the observed heating requirement. We explain the existence of solar flares below the expected nanoflare threshold as follows. They originate in small coronal loops of 200-5000 km, smaller than considered by Parker. Some picoflares show only a partial energy release along a single loop.
000006487 594__ $$aSTCE
000006487 700__ $$aVeronig, A.
000006487 700__ $$aVerbeeck, C.
000006487 700__ $$aSchuller, F.
000006487 700__ $$aVelli, M.
000006487 700__ $$aWarmuth, A.
000006487 773__ $$tSOLARNET Conference: The Many Scales of the Magnetic Sun, Potsdam
000006487 8560_ $$ffrancis.verbeeck@ksb-orb.be
000006487 906__ $$aContributed
000006487 980__ $$aCTALKCONT