2002MNRAS.337..327M

A spatially unresolved velocity feature, with an approaching radial velocity of ~100 km.s^–1 with respect to the systemic radial velocity, in a position-velocity array of [Oiii] 5007-Å line profiles is identified as the kinematical counterpart of a jet from the proplyd LV 5 (158-323) in the core of the Orion nebula. The only candidate in Hubble Space Telescope ( HST) imagery for this jet appears to be a displaced, ionized knot. Also an elongated jet projects from the proplyd GMR 15 (161-307). Its receding radial velocity difference appears at ~80 km.s^–1 in the same position-velocity array.

A `standard' model for jets from young, low-mass stars invokes an accelerating, continuous flow outwards with an opening angle of a few degrees. Here an alternative explanation is suggested which may apply to some, if not all, of the proplyd jets. In this, a `bullet' of dense material is ejected which ploughs through dense circumstellar ambient gas. The decelerating tail of material ablated from the surface of the bullet would be indistinguishable from a continuously emitted jet in current observations.