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Session 41 - T Tauri Stars & Protostellar Regions.
Display session, Wednesday, June 11
South Main Hall,
Weak-line T\,Tauri stars, contrary to classical T\,Tauri stars, no longer possess massive circumstellar disks. In weak-line T\,Tauri stars, the circumstellar matter was either accreted onto the T\,Tauri star or has been redistributed. Disk instabilities in the outer disk might result in the formation of brown dwarfs and giant planets.
Based on photometric and spectroscopic studies of ROSAT sources, we have selected an initial sample of 200 weak-line T\,Tauri stars in the Chamaeleon T association and the Scorpius Centaurus OB association. In the course of follow-up observations we identified visual and spectroscopic binary stars and excluded them from our final list, as the complex dynamics and gravitational interaction in binary systems might aggravate or even completely inhibit the formation of planets (depending on physical separation of the binary components and their mass-ratio). The membership of individual stars to the associations was established from proper motion studies and radial velocity surveys.
Our final sample consists of 70 single weak-line T\,Tauri stars. We have initiated a program to spatially RESOLVE young brown dwarfs and young giant planets as companions to single weak-line T\,Tauri stars using adaptive optics at the ESO 3.6m telescope and HST/NICMOS. In this poster we describe the observing strategy and present first results of our adaptive optics observations.
