Recipes for stellar jets: results of combined optical/infrared diagnostics

Abstract

We examine the conditions of the plasma along a sample of "classical" Herbig-Haro (HH) jets located in the Orion and Vela star forming regions, through combined optical-infrared spectral diagnostics. Our sample includes HH 111, HH 34, HH 83, HH 73, HH 24 C/E, HH 24 J, observed quasi-simultaneously and in the same manner at moderate spatial/spectral resolution. Once intercalibrated, the obtained spectra cover a wide wavelength range from 0.6−2.5 µm, including many transitions from regions of different excitation conditions. This allows us to probe the density and temperature stratification which characterises the cooling zones behind the shock fronts along the jet. From the line ratios we derive the variation of the visual extinction along the flow, the electron density and temperature (n e and T e ), the hydrogen ionisation fraction x e , and the total density n H in the emission region of different lines. The knowledge of such parameters is essential for testing existing jet models and for planning follow-up high-angular resolution observations. From the diagnostics of optical forbidden lines we find, on average, that in the examined jets, in the region of optical emission, n e varies between 50 cm −3 and 3 × 10 3 cm −3 , x e ranges between 0.03 and 0.6, and the electron temperature T e is ∼1.3 × 10 4 K in the HH 111 and HH 34 jets, while it appears to be higher (1.8 × 10 4 K on average) in the other examined jets. The electron density and temperature derived from [Fe ii] lines, turn out to be, respectively, higher and lower in comparison to those determined from optical lines, in agreement with the fact that the [Fe ii] lines arise in the more compressed gas located further from the shock front. An even denser component in the jets, with values of n e up to 10 6 cm −3 is detected using the ratio of calcium lines. The derived physical parameters are used to estimate the depletion onto dust grains of calcium and iron with respect to solar abundances. This turns out to be quite substantial, being between 70% and 0% for Ca and ∼90% for Fe. This leads us to suggest that the weak shocks present in the beams are not capable of completely destroying the ambient dust grains, confirming previous theoretical studies. We then derive the mass flux rates,Ṁ jet , in the flows using two independent methods. Taking into account the filling factor of the emitting gas,Ṁ jet is on average 5 × 10 −8 M yr −1 . The associated linear momentum fluxes (Ṗ jet = v jetṀjet ) are higher than, or of the same order as, those measured in the coaxial molecular flows, where present, suggesting that the flows are jet driven. Finally, we discuss differences between jets in our sample. In general, we find that higher ionisation and electron temperatures are associated with less dense jets. The comparison suggests that the shock mechanism exciting the knots along the flows has the same efficiency in all the examined objects, and the observed differences are consistent with the different densities, and hence cooling rates, found in the vario...

HST/STIS observations of the RW Aurigae bipolar jet: mapping the physical parameters close to the source

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“…The physical properties of the outflow are derived applying the so-called BE technique to the spectra, described, e.g., in BE99 and in Podio et al (2006). Our results can be summarised as follows:…”

“…The results of the BE technique also depend on the adopted abundance of chemical species. Podio et al (2006) showed that the interstellar gas composition determined for the Orion nebula by Esteban et al (2004) led to the most reliable diagnostic results for jets in various regions. Thus, we adopted the same abundance set, assuming RW Aur star formation region has been exposed to the same enrichment processes.…”

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“…However, launching from the stellar surface meets three caveats in explaining observed jets: (i) energetic difficulty to eject >1% of the accretion rate (Cranmer 2009, Ferreira et al 2006, (ii) lack of dust, whereas iron and calcium depletion is measured in several jets (Podio et al 2006, Dionatos et al 2009), (iii) insufficient collimation (Bogovalov & Tsinganos 2001, Fendt 2009, Cabrit 2007 …”