Probing the Solar Atmosphere Through Radiophysics

摘要: The solar corona is a highly ionized plasma which exhibits complex variety of features on different space and time scales [1],[2]. Such range from sub-arcsec to radius show lifetimes the order seconds days, indicating that coronal basically non-homogeneous subject set physical processes, which, one hand, determine such inhomogeneities and, other are affected by them in mutual feedback scheme. recent progress instrumental techniques ground [3] [4], [5], [6] availability multi-wavelength observations have been adding new tiles this frame, but also rendered more puzzling theoretical modelling scales.