Speaker
Description
First Name: Vasanth
Last Name: Anandan
Affiliation: PhD Student, Royal Observatory of Belgium and CmPA/Department of Mathematics, KU Leuven,Belgium
All Authors: Vasanth Anandan1 , Jasmina Magdalenic1,2 , Marilena Mierla1,3, Francesco Carella2, Luciano Rodriguez1, Nancy Narang1, Dana Talpeanu1, Sentamizh Pavai Valliappan1
Abstract: The solar wind is an intriguing phenomenon that influences the heliosphere and has direct implications on the Sun-Earth environment called “Space Weather”. Generally, the solar wind is classified into two types: the fast solar wind originating from open-magnetic field regions (Coronal Holes) and the slow solar wind associated with different sources at the Sun. These source regions may correspond to the large-scale coronal features observed by the Extreme Ultraviolet Imager/Full Sun Imager (EUI/FSI) onboard Solar Orbiter. Using high-resolution observations from EUI/HRI and coordinated observations from PROBA-2/SWAP, STEREO-A/EUVI, SDO/AIA, and EUI/FSI enables us to pinpoint their footpoints location. We also use backmapping of the slow solar wind observed at 1 AU to its corresponding source regions. In addition to that, we perform a detailed analysis of the in-situ solar wind parameters to distinguish between different types of solar wind and their source regions.