Speaker
Description
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 analyzed high temporal frequency visible light observations acquired by Metis coronagraph on Solar Orbiter during the perihelia on 2022 and 2023.
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 also as collapsing loops and outflows as density inhomogeneities (blobs).
These phenomena have been associated with the coronal magnetic structures as derived from a MHD model and they are discussed with theoretical simulations.
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