On the Origin of the Off-Cloud Pre-Main Sequence Stars Found with ROSAT

Details On the Origin of the Off-Cloud Pre-Main Sequence Stars Found with ROSAT On the Origin of the Off-Cloud Pre-Main Sequence Stars Found with ROSAT

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999sf99.proc..403p&link_type=abstract

Star Formation 1999, Proceedings of Star Formation 1999, held in Nagoya, Japan, June 21 - 25, 1999, Editor: T. Nakamoto, Nobeyam

Computer Science

Scientific paper

Several young stars, isolated or in small groups, have recently been found far away from well-known star-forming regions. The origin of these pre-main sequence stars is still under debate. They may have been formed in situ from small cloudlets, or have been ejected with high velocities from the molecular cloud in which they were originally born. We have carried out a search for companions among samples of these isolated pre-main sequence stars, and we use the binary frequency to distinguish between the two proposed ideas. From our analysis of a first sample of 33 T Tauri stars in the wider area of Orion we find a binary frequency of at least 18.2+/-6.7%, which is even higher (factor ~1.5) than for the field star population. This suggests that the majority of the stars may not have experienced ejection, since in that case the stars are expected to be depleted in companions. Furthermore, we have measured stellar rotational periods for isolated T Tauri stars in the direction of Orion, Lupus, Chamaeleon, and TW Hya using UBV-photometry. Among the Lupus sample we find the rotation periods almost equally distributed between around 0.5 and 8 days.

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