Executive Summary : | Magnetohydrodynamic (MHD) oscillations together with mass flows have been discovered ubiquitously in different layers/parts of the solar atmosphere by recent observations sDO/AIA, Hinode/sOT, IRIs, TRACE etc. In this project we aim to analyze the MHD wave's characteristics when mass flows are taking place around the oscillating structure. Wave dampening is important in the context of coronal plasma heating, while appropriate measurement of oscillation amplitude and period of waves play a significant role in plasma diagnostics, e.g., estimation of magnetic field, energy transport coefficients like electrical and thermal conductivities, viscosity etc. which are very hard to detect directly by modern days spectroscopic and imaging observations. However, there are other locations on the sun where field lines are extended in interplanetary space and do not appear to return back another foot point. These regions are referred as coronal holes or plumes (ray like structures basically observed around the polar area of the sun). In these magnetic structures frozen with plasma longitudinal modes of MHD waves have been detected by a number of observations and they have been modeled by slow and fast MHD waves. There are a number of studies concerning the modeling of non-uniform flows with its interaction with MHD waves, e.g., Gruszecki et al. (2008), soler (2019). But modeling of these non-uniforms flows in its separate pattern of longitudinal and transverse profiles and its comparison with uniform profile yet to be discussed. Furthermore, the extension of flow profile beyond the oscillating structure needs to be carried out. Thus, keeping these facts in attention and looking at latest observational findings concerning waves and flows in different part of the solar atmosphere. Using these waves and flow, we develop the mathematical equations and its ultimate connection to coronal heating and diagnostic of the plasma. |