Paper presented to the 3rd Southern African Solar Energy Conference, South Africa, 11-13 May, 2015.
Taking into account the most recent net radiation function
model and five different kinds of heating scenarios for the
upper solar atmosphere, we have defined some regions where
the magnetoacoustical amplification may take place. The
nonlinear equation describing the evolution of fast and slow
magnetoacoustic waves in a heat-releasing completely ionized
plasma has been obtained. The shape and parameters of the
magnetoacoustic pulse that is an automodel solution of this
equation under conditions of magnetoacoustic instability have
been determined
