THE CORONAL STRUCTURE ABOVE SUNSPOTS AND PORES

High-resolution X-ray observations of the solar corona have been used to study the structure above pores and small sunspots. We find that th e lack of X-ray emission previously observed above large spot umbrae i s also seen above pores. As is the case with large spots, the pores ar e surrounded by bright X-ray emitting structures. Using these data we argue that coronal heating requires magnetic field stressing from impo sed motions internal to coronal flux bundles, rather than from displac ement of the flux bundles.