Conclusion: It is highly likely that different magnetic mechanisms are at work in heating the three types of structure that are observed in the solar corona. In X-ray bright points magnetic reconnection
IS probably responsible as separate flux systems reconnect either due to new flux emerging from below the photosphere or due to
so-called "reconnection submergence" (Priest, 1987) as separate magnetic flux elements cancel (Martin, 1986). In coronal holes, magnetic waves can dissipate, either by phase mixing or by resonant absorption. In coronal loops magnetic dissipation in current sheets is likely to be responsible. Such sheets can be produced efficiently at separatrices by shearing mechanisms. Given the limitation of the new selfconsistent model for heating by MHD turbulence, we find it highly encouraging that it predicts a resonable heat flux and microturbulent velocity. In future we look forward to the SOHO observations and to trying to build a new generation of self-consistent coronal heating theories from these ideas.