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Generation, propagation and dissipation of transverse magnetohydrodynamic waves in the solar atmosphere

As the outermost layer of the solar atmosphere, the corona has a temperature of one to several million kelvin. What physical processes heat the coronal plasma to such a high temperature? This is the well-known coronal heating question and is among the top mysteries in modern astronomy. Currently, there are two dominant ideas for the explanation of coronal heating, and one is the dissipation of magnetohydrodynamic (MHD) waves. Transverse MHD waves, such as kink waves and torsional Alfven waves, have been suggested to play an important role in coronal heating. Previous observations have revealed the presence of these waves in the solar atmosphere. However, it is still unclear how these transverse waves are generated and how they propagate from the lower atmosphere to the corona and dissipate the energy there. With high-resolution observations from the 4-meter Daniel K. Inouye Solar Telescope (DKIST) and several advanced solar space telescopes on board the European Solar Orbiter mission and the Chinese ASO-S mission in the next 5 years, we will investigate the detailed generation mechanisms of the transverse waves, track their upward propagation and identify their dissipation signatures. In addition, we plan to perform advanced MHD simulations to correctly interpret the observational results, and accurately evaluate the contribution of these waves to coronal heating.

Date:12 Aug 2022 →  Today
Keywords:Solar atmosphere, Solar corona, Waves
Disciplines:Space plasma physics and solar physics
Project type:PhD project