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dc.contributor.authorBarczynski, Krzysztof
dc.contributor.authorMeyer, Karen A.
dc.contributor.authorHarra, Louise K.
dc.contributor.authorMackay, Duncan H.
dc.contributor.authorAuchère, Frédéric
dc.contributor.authorBerghmans, David
dc.identifier.citationBarczynski , K , Meyer , K A , Harra , L K , Mackay , D H , Auchère , F & Berghmans , D 2022 , ' A statistical comparison of EUV brightenings observed by SO/EUI with simulated brightenings in nonpotential simulations ' , Solar Physics , vol. 297 , no. 10 , 141 .
dc.identifier.otherJisc: 687159
dc.identifier.otherpublisher-id: s11207-022-02074-6
dc.identifier.othermanuscript: 2074
dc.identifier.otherORCID: /0000-0001-6065-8531/work/128096910
dc.descriptionFunding: Open access funding provided by Swiss Federal Institute of Technology Zurich. L.H. and K.B. are grateful to the SNF for the funding of the project number 200021_188390. D.H.M. would like to thank the STFC for support via consolidated grant ST/W001195/1. K.A.M. would like to thank the STFC for support via consortium grant ST/W001098/1.en
dc.description.abstractThe High Resolution Imager (HRIEUV) 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 nonpotential 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 HRIEUV telescope. We applied the same detection method to the simulated energy dissipation maps from the nonpotential simulation to detect simulated brightenings. We detected EUV brightenings with a density of 1.41×10−3 brightenings/Mm2 in the EUI observations and simulated brightenings between 2.76×10−2 – 4.14×10−2 brightenings/Mm2 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 nonpotential 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.
dc.relation.ispartofSolar Physicsen
dc.subjectCorona, quieten
dc.subjectEUV brighteningen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleA statistical comparison of EUV brightenings observed by SO/EUI with simulated brightenings in nonpotential simulationsen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.institutionUniversity of St Andrews. Statisticsen
dc.contributor.institutionUniversity of St Andrews. Applied Mathematicsen
dc.description.statusPeer revieweden

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