Outflow Dynamics, Accretion and Chemical Abundances in YSOs

Details Outflow Dynamics, Accretion and Chemical Abundances in YSOs Outflow Dynamics, Accretion and Chemical Abundances in YSOs

Jul 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001esasp.460..177f&link_type=abstract

The Promise of the Herschel Space Observatory. Eds. G.L. Pilbratt, J. Cernicharo, A.M. Heras, T. Prusti, & R. Harris. ESA-SP 460

Physics

Stars: Formation, Stars: Pre-Main Sequence, Ism: Jets And Outflows, Ism: Clouds, Ism: Molecules

Scientific paper

During the last decade, a big improvement has been done in the comprehension of the low-mass star formation. In particular, the large millimetre telescopes and interferometers have provided important information on the physics and chemistry of infall, outflow (shocks) and photodissociation regions (PDRs). However, key details on how low- and intermediate-mass stars are formed remain still unknown (when bipolar outflow starts?, when the collapse ceases? what determines the mass of the star?, when the PDR is formed?, which is the dominant mechanism in the dispersal of the envelope and accretion disk?...). In this paper we discuss how FIRST observations can contribute to a better understanding of these processes. In particular, we consider that oxygen chemistry (H2O, OH, OI) will constitute an excellent diagnostic for the infall/outflow system. The observation of hydrides will trace the physics and kinematics of the PDRs formed in the later stages of the pre-main sequence evolution. These diagnostics, when applied to statistical studies, could provide the answer to previous questions and a detailed evolutionary sequence for the star formation.

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