Anandan, Vasanth ; Mierla, Marilena ; Magdalenic, Jasmina ; Valliappan Sentamizh, Pavai ; Core Team members, EUI

Seminar presented at Royal Observatory of Belgium on 2025-06-18

Abstract: The solar wind is a hot, supersonic plasma flow from the Sun that shapes the heliosphere and is mainly classified as fast or slow based on speed (Vsw). Fast wind (Vsw > 400 km/s) usually originates from coronal holes, while slow wind (Vsw < 400 km/s) is linked to streamers outside coronal holes. The middle corona (region between 1.5 and 3 solar radii) is thought to be the source region of the solar wind, but the exact origin of the slow wind remains uncertain. It is unclear how closed magnetic field lines open to release trapped plasma. This region is also poorly observed in EUV and white-light. In this seminar I will present a statistical analysis of the large scale coronal structures observed by the Full Sun Imager (FSI)/Extreme Ultraviolet Instrument (EUI) on board the Solar Orbiter (SolO) in its 174 A channel. These structures are of great interest in the context of understanding about the slow solar wind origin and acceleration. In addition to that I plan to study these structures and their connection to the in situ data by using observations from instruments onboard other space missions like STEREO , PROBA2 , and PSP. This will improve our current understanding of the origins of the slow solar wind.

Keyword(s): Solar Wind ; Large Scale coronal structures ; Sun ; Sunspot ; Flares ; Coronal Holes ; Active regions
Funding: 10&OIMPULSE_BOURSE_VASANTH/10&OIMPULSE_BOURSE_VASANTH/10&OIMPULSE_BOURSE_VASANTH