Excitation Mechanisms for Hot Molecular Hydrogen in the Planet-Forming Regions of Protostars

Details Excitation Mechanisms for Hot Molecular Hydrogen in the Planet-Forming Regions of Protostars Excitation Mechanisms for Hot Molecular Hydrogen in the Planet-Forming Regions of Protostars

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21542823b&link_type=abstract

American Astronomical Society, AAS Meeting #215, #428.23; Bulletin of the American Astronomical Society, Vol. 42, p.348

Astronomy and Astrophysics

Astronomy

Scientific paper

The search for gas in the innermost disk regions of classical and weak-lined
T Tauri stars is now several decades old, and has met with some success. Unexpectedly, a large fraction of self-embedded protostars have been found to exhibit quiescent hot molecular hydrogen gas in emission at high spectral resolution. Here, we report for the first time, detections, line ratios, and possible excitation mechanisms (shocks, UV, and/or X-ray) for quiescent near-infrared molecular hydrogen lines found in a sample of protostars in nearby (<300 pc) star-forming regions. Many sources exhibit spatially compact emission lines centered on the young stellar object's radial velocity, with velocity extents consistent with disk emission. Correlations with source X-ray flux, accretion rate, [NeII] line flux, and Br-gamma emission will be explored. Importantly for the line ratio measurements, spectra of the various near-infrared emission lines of hydrogen were acquired simultaneously, using the unique capabilities of the NIRSPEC instrument at the Keck 10-meter.
ACKNOWLEDGEMENTS: Data presented herein were obtained from telescope time allocated to NASA through the agency's scientific partnership with Caltech and U.C. Observing travel support was provided by NASA.

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