Imaging Extended UV H2 Emission Around T Tauri

Details Imaging Extended UV H2 Emission Around T Tauri Imaging Extended UV H2 Emission Around T Tauri

Jul 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005hst..prop10489b&link_type=abstract

HST Proposal ID #10489

Computer Science

Hst Proposal Id #10489 Star Formation

Scientific paper

The interactions between the circumstellar disk, newly-forming star, and bipolar jet outflows play a central role in the process of star formation. These interactions control how disks evolve and dissipate, and, thereby, control the process of planetary system formation. We shall image the UV molecular hydrogen {H2} emission around the pre-main-sequence binary star T Tauri using the ACS SBC {solar blind channel} MAMA detector, thus determining the spatial properties of the H2 emitting regions, and deriving important detailed observational information on the disk-star-jet interaction on scales of order 5 AU. These images will reveal the degree of collimation and opening angles of the innermost parts of the high velocity jets, the shock structure within the jet outflows, the size and morphology of the circumstellar disks, both in emission and in silhouette, and the conditions inside the polar cavities swept clear by Herbig-Haro flows. Fluorescent H2 emission lines dominate the UV spectrum of T Tau. Long-slit {1-D} STIS UV spectra of T Tau show H2 emission with a complex spatial structure extending many arcseconds from the star and the presence of significant shock structures. The H2 must be warm {approx. 2000 K} for the fluorescence to operate. The molecular emission originates in shocks and, perhaps, also from the surfaces of the inner regions of accretion disks.

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