000007135 001__ 7135
000007135 005__ 20250102102655.0
000007135 0247_ $$2DOI$$a 10.1051/0004-6361/202346886
000007135 037__ $$aSCART-2024-0183
000007135 100__ $$aNelson, C. J. 
000007135 245__ $$aSpatial distributions of EUV brightenings in the quiet-Sun
000007135 260__ $$c2024
000007135 520__ $$aThe identification of large numbers of localised transient EUV brightenings, with small spatial scales, in the quiet-Sun corona has been one of the key early results from Solar Orbiter. However, much is still unknown about these events. Here, we aim to better understand EUV brightenings by investigating their spatial distributions, specifically whether they occur co-spatial with specific line-of-sight magnetic field topologies in the photospheric network. EUV brightenings are detected using an automated algorithm applied to a high-cadence (3 s) dataset sampled over ~30 min on 8 March 2022 by the Extreme Ultraviolet Imager's 17.4 nm EUV High Resolution Imager. Data from the Solar Dynamics Observatory's Helioseismic and Magnetic Imager and Atmospheric Imaging Assembly are used to provide context about the line-of-sight magnetic field and for alignment purposes. We found a total of 5064 EUV brightenings within this dataset that are directly comparable to events reported previously in the literature. These events occurred within around 0.015-0.020 % of pixels for any given frame. We compared eight different thresholds to split the EUV brightenings into four different categories related to the line-of-sight magnetic field. Using our preferred threshold, we found that 627 EUV brightenings (12.4 %) occurred co-spatial with Strong Bipolar configurations and 967 EUV brightenings (19.1 %) occurred in Weak Field regions. Fewer than 10 % of EUV brightenings occurred co-spatial with Unipolar line-of-sight magnetic field no matter what threshold was used. Of the 627 Strong Bipolar EUV Brightenings, 54 were found to occur co-spatial with cancellation whilst 57 occurred co-spatial with emergence. EUV brightenings preferentially occur co-spatial with the strong line-of-sight magnetic field in the photospheric network. They do not, though, predominantly occur co-spatial with (cancelling) bi-poles.
000007135 594__ $$aSTCE
000007135 6531_ $$aSun
000007135 6531_ $$acorona
000007135 6531_ $$aEUV brightenings
000007135 700__ $$aHayes, L. A. 
000007135 700__ $$aMüller, D. 
000007135 700__ $$aMusset, S. 
000007135 700__ $$aFreij, N. 
000007135 700__ $$aAuchère, F. 
000007135 700__ $$aAznar Cuadrado, R. 
000007135 700__ $$aBarczynski, K.  
000007135 700__ $$aBuchlin, E.  
000007135 700__ $$aHarra, L. 
000007135 700__ $$aLong, D. M. 
000007135 700__ $$aParenti, S. 
000007135 700__ $$aPeter, H. 
000007135 700__ $$aSchühle, U. 
000007135 700__ $$aSmith, P. 
000007135 700__ $$aTeriaca, L. 
000007135 700__ $$aVerbeeck, C. 
000007135 700__ $$aZhukov, A. N. 
000007135 700__ $$aBerghmans, D.
000007135 773__ $$nid. A236$$pAstronomy & Astrophysics$$v692
000007135 8560_ $$fdavid.berghmans@ksb-orb.be
000007135 85642 $$ahttps://ui.adsabs.harvard.edu/abs/2024arXiv241100467N/abstract
000007135 85642 $$ahttps://www.aanda.org/articles/aa/full_html/2024/12/aa46886-23/aa46886-23.html
000007135 905__ $$ain press to
000007135 980__ $$aREFERD