1,5,- 1INAF, Astrophysical Observatory of Turin, Italy
- 2INAF, Astronomical Observatory of Capodimonte, Italy
- 3Royal Observatory of Belgium, Belgium
- 4University of Florence, Italy
- 5INAF, Astrophysical Observatory of Catania, Italy
In order to investigate the sources and the physical mechanisms for the propagation of the Slow Solar Wind (SSW), it is essential to analyze and modeling solar data in the middle corona which determines the large scale structure and also the origin of the SSW (from 1.5 up to 6 solar radii).
We have analysed high temporal frequency visible light observations acquired by Metis coronagraph on Solar Orbiter during the perihelia on October 2022, April 2023 and September 2024.
In particular, we focused on series of total and polarized Brightness observations lasting for 40 min up to few hours, acquired with a cadence of 20 s and 60 s. The field of view of the observations ranges from 1.7 to 3.5 solar radii.
We have found in these data sets several examples of inflows detected as collapsing loops and density inhomogeneities. We have noticed that this kind of features are observed mainly along the streamer axis and they are not observed in pseudo-streamers.
Similar features have been detected by ASPIICS on PROBA3 from the limb to few solar radia, allowing the study of the dynamics of the corona with a continuous coverage of the field of view.
How to cite: Abbo, L., Andretta, V., Zhukov, A., Mierla, M., Fineschi, S., Romoli, M., Spadaro, D., and Susino, R.: Detection of downflows with Metis and ASPIICS observations, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-13364, https://doi.org/10.5194/egusphere-egu26-13364, 2026.
