Speaker
Description
The dynamic behavior of the solar atmosphere remains one of the most relevant open problems in solar physics, especially regarding energy transport and dissipation. For this reason, the propagation of magnetohydrodynamic (MHD) waves has been used to describe phenomena such as the heating of the solar corona. However, most studies have focused on homogeneous media, even though the solar plasma presents significant inhomogeneities in density, pressure, and magnetic field.
This work proposes to study how these inhomogeneities affect the propagation of linear MHD waves, both in free media and in magnetic flux tubes. The analysis will focus on variations in the wave morphology, their efficiency in energy transport, and the redistribution of energy into kinetic energy, enthalpy, and Poynting flux. The methodology includes the selection of realistic inhomogeneity profiles and the solution of the linearized MHD equations through numerical simulations using the MAGNUS code. Different oscillation modes and boundary conditions will be evaluated to represent typical solar scenarios. This study will help to understand how plasma gradients influence the observable properties of MHD waves, contributing to the improvement of existing theoretical models and facilitating the interpretation of data obtained by high-resolution solar missions.
| Sessions | Wave generation, energy transport, dissipation and heating |
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