Self-consistent model of the quiet solar corona with a wave source of energy

A self-consistent, spherically symmetric model of the solar corona is considered with a heating source connected with linear damping of MHD waves propagating away from the strongly turbulized chromosphere. The regime of the corona is shown to be fully determined by one parameter: the induction B of the coronal magnetic field. If the magnetic field is sufficiently weak, B < B₂ ≅ 2 G, the pressure in the transition layer, the maximum coronal temperature and the altitude of the temperature maximum increase with increasing B, heating is conditioned by the Alfvén and slow magnetosonic waves. If B > B₂, the dependences of the coronal parameters on B become weak due to the regulation by the plasma flow. Coronal heating is conditioned by partial damping of Alfvén waves in this regime, the influence of magnetosonic waves is negligible.