Modelling the wave dynamics of solar atmosphere to study coronal heating

Abstract

Heating in the solar atmosphere has long remained one of the central unsolved problems in solar physics. Despite significant progress in both observational capabilities and theoretical modeling, the precise mechanisms responsible for maintaining the high coronal temperatures continue to be debated. Among the proposed candidates, wave heating — particularly via pmode- driven magnetohydrodynamic (MHD) waves interacting with structured magnetic fields — has attracted increasing interest. In this thesis, we present a comprehensive study of MHD waves through 2.5D MHD simulations to examine the influence of various wave drivers and magnetic field configurations on wave propagation, mode coupling, and energy transport in the solar atmosphere. Our results show that employing a realistic broadband driver for p-mode oscillations produces power spectra peaking around 4 mHz which is in close agreement with observations. Furthermore, we also simulated the solar jets and studied the wave generation and how it is influced under the p-mode oscillations. It was found that p-mode like oscillations can also enhance the high frequency transverse oscillations in chromosphere and generate coronal power spectrum with frequncy peaking at around 3.5-3.7 mHz. These results provide further insight on the role of wave-driven processes in coronal heating and highlight the dynamic coupling between photospheric motions and coronal oscillations.