Abstract
The behaviour of the magnetic field in the solar atmosphere is governed by the equations of MHD rather than the electromagnetism of wires. In particular, the roles of magnetic reconnection are: to create small flares; to trigger large flares; and to release magnetic energy in large flares. Observational evidence for reconnection is reviewed together with recent theory and observation of (post-) flare loops, which enable one to deduce the reconnection electric field from the motion of either the flare loops or Hα ribbons. Also, an account is given of a new unified theory for fast steady-state reconnection which includes the Sweet-Parker, Petschek and Sonnerup-like models as special cases.
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