Abstract
We generalize our analytical and numerical models of the solar flux tube on twisted magnetic-field lines. The basic equations and numerical methods have much in common with those of Murawski et al. (Astron. Astrophys. 577, A126, 2015); the new and important issue is the twisted magnetic-field component that couples explored torsional Alfven and magnetoacoustic waves. In these models we specify a magnetic-flux function and derive general analytical formulas for the equilibrium mass density and a gas pressure. We use the developed models, which can be adopted for any axisymmetric structure with twisted and untwisted magnetic lines, to simulate the MHD waves. These waves are excited by a localized pulse in the azimuthal velocity component that is launched at the top of the solar photosphere. Their propagation through the solar chromosphere and transition region to the solar corona reveals a complex scenario of twisted magnetic-field lines and flows associated with torsional Alfven and magnetoacoustic waves.
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