Effects on UV lines observations of stationary plasma flows confined in coronal loops

The basic "siphon flow" illustrated in a neat cartoon. This is basically a steady flow between the footpoints of a coronal magnetic loop, driven by a pressure differential. No doubt, this is a basic building block in the fluid description of a magnetized stellar atmosphere (including, of course, applications to flare physics). The point of the paper here is to help out with the UV signatures of these processes.