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Dynamics and energetics of coronal loops undergoing decayless oscillations

The Sun, as the nearest star to Earth, has been extensively studied ever since the development of modern Astrophysics. The large number of multi-frequency observations has shed light on many of the phenomena existing in the solar interior and the solar atmosphere, but not without generating a whole range of questions regarding the nature of these processes.

The solar atmosphere is not an assembly of static, clearly defined layers, but is instead a widely dynamic part of the Sun, filled with flows, oscillations and energetic phenomena, like flares. Waves and oscillations are some of the most common observed phenomena across the layers of the solar atmosphere, like the chromosphere and the corona. Of particular interest have been the transverse waves in the solar corona, ever since their discovery in coronal loops in the late 90s, and the revelation of their ubiquitous nature in the solar atmosphere, during the late 2000s.

One of the most important unsolved mysteries in solar physics is the multimillion temperature of the solar corona, with different heating mechanisms being under consideration. The interest in oscillating loops lies in their nature as potential candidates of wave heating of the solar atmosphere. This study focuses on wave heating in coronal loops, which undergo continuous driving. We rely on numerical studies in order to test our theories. The effects of strong drivers and the generation of instabilities on our oscillating loops will be considered. 3D simulations try to shed light on the underlying mechanisms, while post-processing of the results gives us synthetic emission maps, which can be directly compared to the real observations.

Date:1 Oct 2015 →  13 Sep 2019
Keywords:Solar atmosphere, Coronal seismology, magetohydrodynamics, MHD waves
Disciplines:Astronomy and space sciences
Project type:PhD project