Challenges in Forecasting the Evolution of a Distorted CME Observed During the First Close Solar Orbiter Perihelion

• Published in: The Astrophysical journal 2024-07, Vol.970 (1), p.81
• Main Authors: Liberatore, Alessandro, Braga, Carlos R., Temmer, Manuela, Cappello, Greta M., Telloni, Daniele, Liewer, Paulett C., Vourlidas, Angelos, Velli, Marco, Heyner, Daniel, Auster, Hans-Ulrich, Richter, Ingo, Schmid, Daniel, Fischer, David, Möstl, Christian
• Format: Article
• Language: English
• Subjects: Active solar corona; Corona; Coronal holes; Coronal mass ejection; Cylindrical shells; Distortion; Earth; Heliosphere; Magnetic fields; Observatories; Perihelions; Quadratures; Remote sensing; Solar corona; Solar coronal mass ejections; Solar magnetic field; Solar Orbiter (ESA); Solar orbits; Solar wind; Space weather; Spacecraft; Weather forecasting; Wind effects
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ad5003

Coronal Mass Ejections (CMEs), drivers of the most severe Space Weather disturbances, are often assumed to evolve self-similarly during their propagation. However, open magnetic field structures in the corona, leading to higher-speed streams in the ambient solar wind, can be source of strong distortions of the CME front. In this paper, we investigate a distorted and Earth-directed CME observed on 2022 March 25 combining three remote sensing with three in situ observatories at different heliocentric distances (from 0.5 to 1 au). Near quadrature observations by Solar Orbiter and the Solar Terrestrial Relations Observatory revealed a distortion of the CME front in both latitude and longitude, with Solar Orbiter observations showing an Earth-directed latitudinal distortion as low as ≈6 R ⊙ . Near-Earth extreme-ultraviolet observations indicated the distortion was caused by interaction with faster wind from a nearby equatorial coronal hole. To evaluate the effect of the distortion on the CME's propagation, we adopted a three-point-of-view graduated cylindrical shell (GCS) fitting approach. For the first time, the GCS results are combined with an additional heliospheric single-viewpoint that looks further out in the heliosphere, revealing a deceleration in the CME before reaching ≈100 R ⊙ . The CME geometry and velocity determined by this enhanced GCS are used to initialize a drag-based model and a WSA-Enlil MHD model. The estimated times of arrival are compared with in situ data at different heliocentric distances and, despite the complexity of the event, the error in the arrival times at each spacecraft results much lower (≈4 hr error) than the typical errors in literature (≈8–10 hr).