Anandan, Vasanth ; ; Magdalenic, Jasmina ; ; Mierla, Marilena; ; Rodriguez, Luciano; ; Valliappan, Sentamizh Pavai; ; Carella, Francesco ; ; Talpeanu, Dana.

Talk presented at The XVIIIth Hvar Astrophysical Colloquium, Hvar, Croatia on 2025-09-18

Abstract: The continuous flow of charged particles that travels from the Sun into the heliosphere is known as the solar wind. In general, there are two main categories of solar wind: fast and slow. While the fast solar wind is known to originate in coronal holes, the source location and mechanisms involved in the slow solar wind's formation are still strongly discussed. Here, we present a thorough analysis of four of the large-scale coronal structures”, observed at equatorial regions in 2022, possible source regions of the slow solar wind. The large-scale structures were observed by the Solar Orbiter's Extreme Ultraviolet Imager/Full Sun Imager |(SolO/EUI). The SolO/EUI observations cover a larger field of view and have higher resolution than any other EUV instrument to date, allowing us to clearly observe faint coronal structures. Using coordinated observations from SolO, STEREO, PROBA2, and Parker Solar Probe, we investigate main characteristics of the large-scale coronal structures such as source locations, their complex dynamic behaviour, and the associated physical mechanisms responsible for sourcing the slow solar wind into the heliosphere.

Keyword(s): Solar Wind ; Coronal Structures ; Streamers ; Coronal Fans
Funding: 10&OIMPULSE_BOURSE_VASANTH/10&OIMPULSE_BOURSE_VASANTH/10&OIMPULSE_BOURSE_VASANTH