A 3-mode variable ejection velocity, precessing jet model for HH 30

Details A 3-mode variable ejection velocity, precessing jet model for HH 30 A 3-mode variable ejection velocity, precessing jet model for HH 30

Jun 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007a%26a...468..613e&link_type=abstract

Astronomy and Astrophysics, Volume 468, Issue 2, June III 2007, pp.613-616

Astronomy and Astrophysics

Astrophysics

6

Ism: Herbig-Haro Objects, Ism: Individual Objects: Hh30, Ism: Jets And Outflows, Stars: Formation

Scientific paper

Context: HH 30 is a Herbig-Haro (HH) jet showing a chain of aligned knots (with knots covering a range of sizes and knot separations), pointing towards what appears to be a highly fragmented “head”. The chain of knots is detected out to ~140'', and the head is an elongated group of knots centred at a distance of ~290'' from the source. Aims: In the paper of Anglada et al. (2006, A&A, submitted), it is suggested that this jet is the result of a multi-period variable velocity ejection, and also having a precession of the outflow axis. The question that we address in our paper is whether or not this ejection variability results in a leading working surface with the high fragmentation of the “head” of the HH 30 jet. Methods: In order to do this, we take at face value the parameters calculated by Anglada et al. (2006) for the ejection variability and the precession and use them to compute a 3D, radiative jet simulation. Our simulation includes a treatment of the non-equilibrium ionization state of the gas, and allows us to compute synthetic emission line maps, which can be compared directly with previously published images of HH 30. Results: We find that our simulation does produce a leading working surface with a striking resemblance to the head of HH 30. We obtain a fragmented emission structure with an extent both along and across the outflow axis that agrees well with the observed jet head. Conclusions: It then appears to be clear that the variable ejection implied by the chain of knots close to the HH 30 source has a direct effect on the head of the jet, producing a highly fragmented structure that is comparable with observations. This is the first time that such a connection has been proven for an HH outflow.

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