Abstract
In previous chapters, we studied post-reconnection processes resulted from interaction of photospheric flux tubes, embedded predominantly in nonmagnetic environment. Higher in the atmosphere, magnetic field preserves its filamentary structures, but is surrounded by low beta-magnetized plasma. In this chapter, we will study post-reconnection processes occurring in the arbitrarily magnetized plasma. We will see that in this case a reconnection triggers various branches of MHD shocks, and cumulation of energy occurs higher in the atmosphere reaching coronal heights and beyond. We are still dealing here with the atmosphere above the rarefied ensembles of flux tubes. Thus imprint of quiet sun at coronal heights is the most expected outcome of post-reconnection processes occurring at all levels. Moreover, these processes seem to be the reliable energy source to fuel the fast solar wind which is rooted in coronal holes outside sunspots and active regions.
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