Water in Protoplanetary Disks

Details Water in Protoplanetary Disks Water in Protoplanetary Disks

Aug 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007noao.prop..179c&link_type=abstract

NOAO Proposal ID #2007B-0179

Computer Science

Scientific paper

Detailed studies of the gas at planet-forming radii in protoplanetary disks are required in order to understand the key chemical, thermal and dynamical processes important for planet formation. Recent spectra from Spitzer-IRS show that emission from rotational lines of H_2O are common in the mid-infrared spectra of classical T Tauri stars, making water a interesting probe of gas at AU radial distances. For example, water is not expected to be abundant in the temperature inversion region of the disk atmosphere where the emission arises. This may indicate strong vertical mixing (which brings water from near the disk midplane), a process with important consequences for understanding the origin of the Solar system. A key issue for any comparison to theoretical models is the radial location of the meuasred water. We propose to obtain high-resolution TEXES spectra of a sample of T Tauri stars to measure velocity profiles of select H_2O lines. These data will confirm the disk origin of the emission, determine the radii at which the water gas resides, and constrain the radial variation of gas temperature and column density.

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