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A. Donar, W. Herbst (Wesleyan University)
The upcoming Space Interferometry Mission (SIM) will provide the first opportunity to detect planets in orbit around pre-main sequence stars, and possibly answer a variety of questions concerning the frequency and dynamics of giant planet formation. Capable of measuring stellar positions to an accuracy of a few \muarcsec, SIM will be able to detect the tiny shift in the photocenter of a star induced by a planetary companion. However, studies of the variability of T Tauri stars have shown them to be covered with large spots, which themselves could cause shifts in the photocenter, potentially masking those due to an orbiting planet. We present the results of preliminary work aimed at both identifying low amplitude variables which would minimize the introduction of astrometric noise, and modeling the effects of spots on the location of the photocenter. Towards that end, we have obtained new I-band photometry of five WTTS: LkCa 2, LkCa 14, TAP 26, TAP 49 and TAP 50. We have also investigated the distribution of inclination angles of TTS in the Taurus-Auriga association and found it to be random. This work was inspired by a SIM key project entitled ``The Search for Young Planetary Systems and The Evolution of Young Stars'' whose lead PI is C. Beichman of JPL.