000005854 001__ 5854
000005854 005__ 20221019090146.0
000005854 037__ $$aSCART-2022-0099
000005854 100__ $$aBarczynski, K. 
000005854 245__ $$aA Statistical Comparison of EUV Brightenings Observed by SO/EUI with Simulated Brightenings in Non-potential Simulations
000005854 260__ $$c2022
000005854 520__ $$aThe High Resolution Imager (HRI_EUV) telescope of the Extreme Ultraviolet Imager (EUI) instrument onboard Solar Orbiter has observed EUV brightenings, so-called campfires, as fine-scale structures at coronal temperatures. The goal of this paper is to compare the basic geometrical (size, orientation) and physical (intensity, lifetime) properties of the EUV brightenings with regions of energy dissipation in a non-potential coronal magnetic field simulation. In the simulation, HMI line-of-sight magnetograms are used as input to drive the evolution of solar coronal magnetic fields and energy dissipation. We applied an automatic EUV brightening detection method to EUV images obtained on 30 May 2020 by the HRI_EUV telescope. We applied the same detection method to the simulated energy dissipation maps from the non-potential simulation to detect simulated brightenings. We detected EUV brightenings with density of 1.41x10^{-3} brightenings/Mm^2 in the EUI observations and simulated brightenings between 2.76x10^{-2} - 4.14x10^{-2} brightenings/Mm^2 in the simulation, for the same time range. Although significantly more brightenings were produced in the simulations, the results show similar distributions of the key geometrical and physical properties of the observed and simulated brightenings. We conclude that the non-potential simulation can successfully reproduce statistically the characteristic properties of the EUV brightenings (typically with more than 85% similarity); only the duration of the events is significantly different between observations and simulation. Further investigations based on high-cadence and high-resolution magnetograms from Solar Orbiter are under consideration to improve the agreement between observation and simulation.
000005854 594__ $$aSTCE
000005854 6531_ $$aCorona, quiet 
000005854 6531_ $$aObservation
000005854 6531_ $$aSimulation
000005854 6531_ $$aEUV brightening
000005854 6531_ $$aEUI
000005854 700__ $$aMeyer, K. A. 
000005854 700__ $$aHarra, L. K. 
000005854 700__ $$aMackay, D. H. 
000005854 700__ $$aAuchère, F.
000005854 700__ $$aBerghmans,  D.
000005854 773__ $$pastronomy & Astrophysics$$y2022
000005854 8560_ $$fdavid.berghmans@observatoire.be
000005854 85642 $$ahttps://arxiv.org/abs/2210.09129 
000005854 905__ $$aaccepted to be published in
000005854 980__ $$aREFERD