Molecular chemistry in protostellar disk winds and observational predictions for Herschel and ALMA

Details Molecular chemistry in protostellar disk winds and observational predictions for Herschel and ALMA Molecular chemistry in protostellar disk winds and observational predictions for Herschel and ALMA

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..280p.389y&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

Astronomy

Scientific paper

The origin of protostellar jets, and their role in extracting angular momentum from the accreting system, remain as major open questions in star formation research. The presence of abundant molecules such as CO, H_2, H_2O, SO and SiO, in the youngest class 0 jets (see eg. Taffala et al. 2010) provides an important new challenge for proposed ejection models. Here we explore the possibility that the jet may trace a dusty magneto-hydrodynamic (MHD) centrifugal disk wind launched beyond the dust sublimation radius of 0.1-0.2 AU. The coupled ionization, chemical, and thermal evolution along dusty flow streamlines is computed for a prescribed MHD disk wind solution (Casse & Ferreira 2000), using a method developed for magnetized shocks in the interstellar medium (Flower and Pineau des Forets 2003). We consider 134 species, including gas-phase atoms and molecules (neutral and singly ionized) as well as species on grain icy mantles and inside grain cores. The chemical network consists of 1143 reactions including neutral-neutral and ion-neutral reactions, photo-ionization and photodissociation, recombination with electrons, charge exchange, cosmic ray induced desorption from grains, and sputtering of grain mantles and cores by neutral impact. Heating by ambipolar diffusion, and irradiation by coronal X-rays and far-ultraviolet photons from accretion shocks, are included (see Panoglou et al. 2011), as well as an improved treatment of self-shielding of H_2 and CO (Yvart et al. 2011). We present predictions for the most abundant molecules in the MHD disk wind, and emission maps and line profiles in H_2, CO, and (if available) H_2O. These predictions are compared with observed characteristics from ground-based and space-borne infrared and submm telescopes (eg. Spitzer, Herschel) and with future ALMA capabilities.

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