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OPTICAL EMISSION LINE PROFILES OF THE LV KNOTS (PROPLYDS) IN ORION

Compact emission line “LV knots” discovered by Laques and Vidal (1979) in the Orion Nebula (M 42) are found to spatially coincide with some of the “proplyds” discovered by O’Dell, Wen and Hu (1993) in their HST images. We therefore attempt to reproduce the line profiles observed for the LV knots with the photoevaporated disk/wind interaction model that has been developed by Henney et al. (1996) for modelling the proplyds. In particular, we present high resolution [O iii] 5007Å line profiles of the knots LV 1 (OW 168–326E), LV 2 (OW 167–317), LV 3 (OW 163–317) and LV 5 (OW 158–323), and also of another faint emission line knot (OW 171–334) in the vicinity of θ1 Ori C. Good agreement between the theoretical predictions and the observed line profiles is found for three of the knots, in which most of the main features of the line profiles are reproduced by the model. A partial, qualitative agreement is also found for the other knots. From these results we conclude that the model of a photoevaporated disk wind interacting with the wind from θ1 Ori C at least partially succeeds in reproducing the line profiles of the proplyds associated with the LV knots.