Probing X-ray photoevaporative winds through their interaction with   ionising radiation in cluster environments: the case for X-ray proplyds
  We show that if young low mass stars undergo vigorous X-ray driven disc winds, these may be detected in clusters through their interaction with ionising radiation from massive stars. We argue that in the ONC (Orion Nebula Cluster) one should see $\sim$ 10s of `X-ray proplyds' ( objects with optically imaged offset ionisation fronts) in the range $0.3-0.6$pc from $\theta_1$C Ori (the dominant O star in the ONC). Such objects lie outside the central `FUV zone' in the ONC where proplyds are instead well explained by neutral winds driven by external Far Ultraviolet (FUV) emission from $\theta_1$C. We show that the predicted numbers and sizes of X-ray proplyds are compatible with those observed and that this may also explain at least some of the far flung proplyds seen in the Carina nebula. We compare the sizes of observed proplyds outside the FUV region of the ONC with model predictions based on the current observed X-ray luminosities of these sources ( bearing in mind that the current size is actually set by the X-ray luminosity a few hundred years ago, $\sim$ the flow time to the ionisation front). We discuss whether variability on this timescale can plausibly explain proplyd size data on a case by case basis. We also show that the predicted radio free-free emission signature of X-ray proplyds is readily detectable. Monitoring is however required to distinguish such emission from non-thermal emission from active coronae. We also predict that it is only at $> 1$ pc from $\theta_1$C that the free-free emission from such offset ionised structures would be clearly distinguishable from an externally driven ionised disc wind. We argue that the fortuitous proximity of massive stars in the ONC can be used as a beacon to light up internally driven X-ray winds and that this is a promising avenue for observationally testing X-ray photoevaporation. 
C. J. Clarke and James. E. Owen
astro-ph.SR