Photospheric network as the energy source for the quiet-Sun corona

We propose a mechanism for the formation of a magnetic energy avalanche bas ed on highly dynamic phenomena within the ubiquitous small-scale network ma gnetic elements in the quiet photosphere. We suggest that this mechanism ma y provide constant mass and energy supply for the corona and fast wind. Con stantly emerging from sub-surface layers, flux tubes collide and reconnect generating magneto-hydrodynamic shocks that experience strong gradient acce leration in the sharply stratified photosphere/chromosphere region. Acousti c and fast magnetosonic branches of these waves lead to heating and/or jet formation due to cumulative effects (Tarbell et al., 1999). The Alfven wave s generated by post-reconnection processes have quite a restricted range of parameters for shock formation, but their frequency, determined by the rec onnection rate, may be high enough (omega similar or equal to 0.1-2.5 s(-1) ) to carry the energy into the corona. We also suggest that the primary ene rgy source for the fast wind lies far below the coronal heights, and that t he chromosphere and transition region flows and also radiative transient fo rm the base of the fast wind. The continuous supply of emerging magnetic fl ux tubes provides a permanent energy production process capable of explaini ng the steady character of the fast wind and its energetics.