Ionization and density along the beams of Herbig-Haro jets
Francesca Bacciotti 1 and
Jochen Eislöffel 2,3,4
Received 1 August 1997 / Accepted 29 October 1998
Physical properties of several well-known Herbig-Haro jets are investigated using an improved version of the spectroscopic diagnostic technique originally developed by Bacciotti et al. (1995). The procedure allows one to derive in a model-independent way the hydrogen ionization fraction in regions of low excitation. The ionization fraction, the electron and gas density, and the average excitation temperature are derived for various positions along the flows.
We find that the hydrogen ionization fraction, with typical initial values of 20-30%, generally decreases along the whole jet or along parts of the flow, following well-defined recombination laws. These results are consistent with the idea that the gas is initially ionized in the jet acceleration region, and then slowly recombines while traveling away from the source. If shocks along the jet beam are present, they can at most have a minor contribution to the ionization of the gas, as apparent in HH 34 and in the first ,of the HH 46/47 jet, where the ionization fraction decreases almost monotonically. In the jets in which re-ionization episodes occur (i.e. HH 24C/E and HH 24G), the ionization fraction suddenly increases and then gently decays downstream of the re-ionization event. Both findings apparently disfavour a mini-bow shock interpretation for the production of the ionization of the beam.
The total densities derived from the ratio between the electron density and the ionization fraction range from about to a few cm-3. Without applying a correction for shock compression, the average mass loss rate varies from 3.8 (in the HL Tau jet) to 1.2 M yr-1 (in HH24 G), while momentum supply rates vary between 1.6 (in the HL Tau jet) and 3.1 M yr- 1 km s-1 (in HH 24G). Taking shock compression into account, these values may be reduced by a factor 3-5.
Key words: ISM: kinematics and dynamics ISM: jets and outflows stars: formation line: formation
Present address: School of Cosmic Physics, Dublin Institute for Advanced Studies, 5 Merrion Square, Dublin 2, Ireland (email@example.com)
Send offprint requests to: F. Bacciotti
© European Southern Observatory (ESO) 1999
Online publication: February 23, 1999