Locating Disks, Accretion Flows, and Outflows in Close Binary T Tauri Stars

Details Locating Disks, Accretion Flows, and Outflows in Close Binary T Tauri Stars Locating Disks, Accretion Flows, and Outflows in Close Binary T Tauri Stars

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6735g&link_type=abstract

HST Proposal ID #6735

Computer Science

Hst Proposal Id #6735 Cool Stars

Scientific paper

Although the standard model for star formation is based on single stars, we now know that most T Tauri stars are in multiple star systems with the majority having separations less than 100 AU, the size typically inferred for a circumstellar disk. Planetary Camera {PC} observations of a few T Tauri binary stars in Cycle 4 have revealed a particularly surprising result: contrary to the standard model for T Tauri stars, the secondary stars have ultra-violet {UV} but no infrared {IR} excesses. We interpret this as a signature of diskless accretion, a phenomenon previously unobserved in T Tauri stars. Furthermore, this result suggests that planetary formation is unlikely to occur around these close secondary stars. In Cycle 6, we propose to use the Planetary Camera aboard HST to carry out a high resolution imaging survey of T Tauri binary stars at a variety of wavelengths. These observations will reveal whether diskless accretion onto close {<= 100 AU} secondary stars is the norm. This would indicate the accretion of material with low angular momentum compared to the binary star and would thereby constrain binary star formation models. An additional outcome of this study is a unique test of the theoretical pre-main sequence tracks, as the components of close binary T Tauri stars are approximately coeval.

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