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Astron. Astrophys. 324, 656-660 (1997)

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Optical emission line profiles of the LV knots (proplyds) in Orion

W.J. Henney 1, J. Meaburn 2, A.C. Raga 1 and R. Massey 2

1 Instituto de Astronomía, UNAM, Apartado Postal 70-264, 04510 México D.F., México
2 Department of Physics and Astronomy, The University, Manchester M13 9PL, UK

Received 31 July 1996 / Accepted 11 December 1996


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 [3 ] 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 [FORMULA]  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 [FORMULA]  Ori C at least partially succeeds in reproducing the line profiles of the proplyds associated with the LV knots.

Key words: ISM: regions – ISM: Individual: Orion nebula – ISM: jets and outflows – line: profiles – stars: pre-main-sequence

© European Southern Observatory (ESO) 1997

Online publication: May 26, 1998