5862 20230201160354.0 POSTER-2022-0041 Harra, Louise Intriguing coronal upflows at the edge of a sunspot - what causes it and can it become part of the solar wind? 2022 2022-09-12 Poster P14 in the conference abstract book During the Solar Orbiter perihelion on March 7 2022, Solar Orbiter observed an active region (NOAA 12960) with EUI high resolution imagers (HRI) and the Hinode EUV Imaging Spectrometer. During the high cadence HRI observations, there was a persistent blue-shifted upflow area in the active region. Similar upflows are often seen at the edges of active regions in the plage areas, and can contribute to the slow solar wind. In the case of AR12960, the upflow region is located unusually close to the strong magnetic field of the sunspot umbra, dominantly in the penumbra region. We analyse both imaging and spectroscopy data, and carry out magnetic modelling to determine if it is possible that this upflow region can make its way into the slow solar wind. The 2 second cadence, high spatial resolution HRI data allow us to explore all the small scale features and dynamics within the upflow region including small loops and small scale transients ‘dots’. STCE Sun corona EUI Barczynski, Krzysztof Mandrini, Cristina Brooks, Dave Cristiani, German Sterling, Alphonse Schühle, Udo Berghmans, D. Auchere, Frederic Azar Cuadrado, Regina Buchlin, Eric Chitta, Pradeep Kraaikamp, E. Long, David Mandel, Sudip Parenti, Susanna Peter, Hardi Rodriguez, L. Smith, Phil Teriaca, Luca Verbeeck, C. Zhukov, A. 8th Solar Orbiter Workhop, Belfast (UK) david.berghmans@observatoire.be CPOSTER