Shrivastav, A. K. ; Pant, V. ; Berghmans, D. ; Kumar, R. ; Zhukov, A. N. ; Van Doorsselaere, T. ; Petrova, E. ; Banerjee, D. ; Lim, D. ; Verbeeck, C.

published in Solar Orbiter Science Nuggets, 30/07/2025 issue #66 (2025)

Abstract: The long-standing problem of coronal heating focuses on probing sources that can continuously supply energy to sustain million-degree temperatures. Magnetohydrodynamic (MHD) waves play a crucial role because their dissipation in the solar corona can supply the necessary energy to compensate for radiative losses. Moreover, MHD waves offer an effective tool for diagnosing local physical conditions through coronal seismology. Elucidating the characteristics of MHD waves across various coronal regions and at different spatial scales is crucial in the context of coronal heating and its driving mechanisms. Decayless transverse kink waves are a type of MHD wave mode in coronal loops with no significant decay in the wave amplitude over multiple cycles. These are omnipresent in active regions [1] which makes them a viable candidate for coronal heating [2]. Additionally, they provide an essential tool to diagnose coronal magnetic fields in the quiet active region corona [3] .

Keyword(s): Solar Orbiter ; EUI ; waves
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