Abstract
The Orion nebula proplyd 168-326 (LV 1) consists of a pair of photoevaporation flows, one from the circumstellar disk of each member of a protostellar binary system. The two flows collide at mildly supersonic velocities, producing a dense interproplyd shell bounded by two weak shocks, while further interactions occur between the individual photoevaporation flows and the stellar wind from the ionizing star θ1 Ori C . I show how observations of the interproplyd shell allow the geometry of the binary system to be usefully constrained and investigate to what extent the weak shocks may directly contribute to the observed shell emission at optical and radio wavelengths.
