Astronomy and Astrophysics – Astrophysics
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..280p.110c&link_type=abstract
The Molecular Universe, Posters from the proceedings of the 280th Symposium of the International Astronomical Union held in Tole
Astronomy and Astrophysics
Astrophysics
Scientific paper
The launching process of jets from young stars is still a major open question in astrophysics. Jets remove angular momentum, allowing accretion onto the protostar. However, it is still unclear whether the launch region of the jet corresponds to the inner edge of the accretion disk at ≤ 0.1 AU, the outer disk at ge; 1 AU , or even the star itself. Most investigations so far of the jet origin have been made in atomic microjets from optically visible T Tauri stars, thanks to the high angular resolution available in the optical range. Recently, the advent of sub-arcsecond resolution with submm interferometers has opened a new window by allowing studies of the jet base in much younger (Class 0) protostars, where only molecules such as CO, SiO, H_2O are detected. In particular, we have shown with IRAM-PdBI that SiO forms in the bipolar HH 212 jet within a timescale of at most 25 years, and is optically thick and close to LTE (Codella et al. 2007, Cabrit et al. 2007). Due to this high optical depth, only lower limits to the SiO abundance could be derived. Here we will present new CO observations of the HH212 jet at 0.3'' resolution with IRAM-PdBI that allow us to better constrain the SiO abundance and the mass-flux in this jet. Our results will be compared with two classes of chemical models for the SiO formation; gas-phase synthesis in dust-free protostellar winds (Glassgold et al. 1991), and dust sputtering and fragmentation in shocks (Gusdorf et al. 2008a,b; Guillet et al. 2009, 2011). Implications for the launch zone of protostellar jets will be discussed.
Cabrit Silvie
Codella Claudio
Gueth Frédéric
Taquet Vianney
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