We present 2D hydrodynamic simulations of the interaction between an ionized photoevaporation flow from a proplyd and a stellar wind from a hot star. We consider both the case of a fully supersonic wind and the case of a wind that passes through a global shock to become subsonic before reaching the proplyd. We compare the results of our simulations with the observed properties of the standoff bowshocks in the Orion proplyds, finding good agreement with the supersonic case for the closer-in proplyds. This allows the momentum flux, $\dot{M} V$, of the stellar wind of \thC\ to be constrained. More distant proplyds do not fit this model but may be explained by the subsonic case, offering the prospect of using the proplyds to probe the position of the inner shock in the wind from \thC. Comparison of predicted silicate dust emission with published mid-infrared imaging provides evidence that submicron-sized grains are underabundant in the proplyd flows by an order of magnitude.
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William J. Henney (w.henney@astrosmo.unam.mx)Last modified: Tue Aug 28 13:01:00 CDT 2001