Propagation of Slow Body Waves in Nonuniform Photospheric Waveguides

Understanding the fluctuations in plasma within magnetic structures, including solar sunspots and pores, is largely dependent on magnetohydrodynamic (MHD) oscillations. In order to understand guided wave phenomena, which aid in deciphering the complex dynamics of solar and astrophysical plasmas, these oscillations are fundamental. In order to improve space weather forecasting, solar atmosphere modeling, and controlled fusion research, scientists can examine energy flow, plasma instabilities, and magnetic field interactions by examining MHD waves. The rhythmic characteristics of the slow body MHD waves in magnetic waveguides with irregular profiles — often seen as pores or sunspots in the solar photosphere are examined in this study. A Sturm–Liouville problem with Dirichlet boundary conditions imposed at the waveguide boundary is solved numerically to obtain the eigenvalues and eigenfunctions of these modes in an isothermal plasma environment. Inhomogeneities in density (or pressure) and magnetic field significantly affect the spatial structure of the waves, the findings of this paper, and higher-order modes are especially vulnerable to these changes. Furthermore, the results highlight that identifying modes only by visual evaluation could lead to erroneous interpretations of their traits.