Probing Chemistry in Disks through Emission of Molecules such as SiO, C_2H_2 and HCN

Details Probing Chemistry in Disks through Emission of Molecules such as SiO, C_2H_2 and HCN Probing Chemistry in Disks through Emission of Molecules such as SiO, C_2H_2 and HCN

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006noao.prop..455k&link_type=abstract

NOAO Proposal ID #2006B-0455

Physics

Scientific paper

We propose to use high resolution mid-infrared spectroscopy to observe the disks around three young stars in lines of a wide variety of molecules (acet, HCN, nhhh, SiO, methane, CS, HNCO and \chhh), in order to study the chemistry as a function of disk radius in the inner 10 AU. It is known from CO observations that the material inside that radius is hot, indicating that a rich chemistry should ensue since most of the molecules are in the gas phase. Spectroscopy of mm wavelength lines tends to sample only cool gas, and previous IR spectroscopy is too low resolution to detect weak lines. Our observations will cover a wide range of energy levels and will resolve line profiles, both of which will help us associate different species with different parts of the inner disks. In addition, both the profiles and whether the lines are in emission or absorption will allow us to determine the disk orientation

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