Speaker
Description
First Name: Yuhang
Last Name: Gao
Affiliation: Peking University; KU Leuven
All Authors: Yuhang Gao, Hui Tian, Richard Morton, Tom Van Doorsselaere, Daye Lim, Mingzhe Guo
Abstract: Polar coronal holes are the primary source regions of high-speed solar wind, yet the acceleration and heating mechanisms operating there remain poorly understood. Transverse magnetohydrodynamic (MHD) waves, especillay the propagating kink waves, are considered key candidates for coronal heating and solar wind acceleration. However, previous low-cadence observations (≥12 s) typically detected wave periods longer than 100 s, yielding insufficient energy to account for these processes. Here, we analyzed high spatio-temporal resolution observations from the Extreme Ultraviolet Imager (EUI) aboard Solar Orbiter in the 17.4 nm passband (cadence of 5 s and pixel size of 0.21 Mm) to investigate kink waves propagating along plumes in a polar coronal hole. Within heights of 8–40 Mm above the solar surface, we extracted horizontal slices to construct time–distance maps, revealing numerous plume structures exhibiting clear transverse oscillations. Using an automatic detection algorithm, we identify 1889 wave events, many with periods shorter than 100 s. Power spectral analysis shows pronounced peaks at high frequencies (≥10 mHz), which are undetectable in lower-cadence data. These high-frequency waves contribute substantially to the total wave energy, revealing an abundant population of high frequency kink waves that may play a crucial role in coronal heating and solar wind acceleration.