Characterizing the Planet Forming Region Around V1331 Cyg
Abstract
Observations of the gaseous component of inner disks (i.e., in the planet formation region) can provide unique insights into the roles that disks play in star and planet formation, by probing the physical and chemical conditions in disks. Recent Spitzer observations show that emission from water, OH, and organic molecules (C2H2, HCN, and CO2) are commonly present in the mid-IR spectra of T Tauri stars, and point to an origin in the terrestrial planet region of the disk (T 300-800 K, R 0.5 - few AU). We present L-band spectra at high resolution (R = 20,000) of V1331 Cyg, an intermediate mass object (spectral type A8-G5) that shows strong OH and water emission. At the high velocity resolution of our observations, we can resolve individual emission lines despite the high line density of the emission. By comparing the observed spectra with synthetic disk models we probe the nature of the accretion mechanism in the disk from the temperature, column density, and line broadening of the water emission that is present. We also model the strong OH emission in our observations to a) probe the disk photochemistry from the abundance ratio with water, and b) characterize the OH excitation mechanism from the ratio of different line strengths. Finally, we open a new window onto the nature of disk chemistry by detecting or setting detection limits on organic species (e.g. HCN, C2H2, H2CO) that may be present in the inner disk region.
- Publication:
-
American Astronomical Society Meeting Abstracts #215
- Pub Date:
- January 2010
- Bibcode:
- 2010AAS...21542808D