2002ApJ...566..315H

We have obtained Hubble Space Telescope (HST) Space Telescope Imaging Spectrometer high-resolution spectra of the Orion proplyd LV 2 in the C III doublet at 1906.68 and 1908.73 Å. New images at the 6 cm wavelength with MERLIN complement earlier HST images at a similar spatial resolution. This object is one of the closest proplyds to θ¹ Ori C, the source of the photoionizing and photoevaporating radiation. Combining the spectra with the HST images and detailed theoretical models has allowed a determination of the mass-loss rate as 8.2x10^–7 M_☉ yr^–1 ±10%. This rate of mass loss is used to address the conundrum of the continued existence of proplyds. Even though they should be photoevaporated in only about 10⁵ yr, there is no evidence for their destruction. It is concluded that the only explanation is that the age of θ¹ Ori C is less than 10⁵ yr. These spectra and previously unpublished ground-based spectra in [O III] also show the presence of a monopolar microjet, redshifted by about 100 km s^–1 with respect to the systemic velocity. This jet is more visible in the 6 cm MERLIN images than in HST images, and this image together with the spectra are used to determine the flow parameters for the jet. Our spectra also include the stand-off shock that lies between LV 2 and θ¹ Ori C. This is the result of the high-velocity wind coming from the hot star θ¹ Ori C with the low-velocity wind coming from the proplyd. As expected, this shock is at rest with respect to the two objects.