The Kelvin-Helmholtz Instability in the Fan-spine Magnetic Topology in the Solar Corona | Sudheer K. Mishra
Affiliation
Indian Institute of Technology (BHU)
Main category
Natural Sciences (Astrophysics and Astrononmy)
Caption
Using multi-wavelength imaging observation obtained from the Atmospheric Imaging Assembly (AIA) onboard Solar Dynamics Observatory (SDO), we study the evolution of Kelvin-Helmholtz (K-H) instability in a fan-spine magnetic topology. This fan-spine configuration is situated near the Active Region 12297 and is rooted in a nearby sunspot. The two layers of the cool plasma flows lift up from the fan plane in parallel and interact with each other at the maximum height of the elongated spine in the lower corona. The first layer of the plasma flow (F1) moving with a slow velocity (5 km/s) reflected from the spine’s field lines. Subsequently second layer of plasma flow (F2) with impulsive velocity (114-144 km/s) interacts with the first layer at the maximum height and generating the shear motion ,
Further reading
Link to the European Solar Physics Online Seminars (ESPOS) webpage:
https://espos.stream/2021/01/14/Mishra/
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