Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...197.1005k&link_type=abstract
American Astronomical Society, 197th AAS Meeting, #10.05; Bulletin of the American Astronomical Society, Vol. 32, p.1413
Astronomy and Astrophysics
Astronomy
Scientific paper
It is now a commonly accepted fact that all or nearly all T Tauri stars (TTS) in the Taurus-Auriga star-forming region form in binary systems (Leinert et al. 1993; Ghez et al. 1993; Koehler & Leinert 1998). This means that the binary frequency among TTS in Taurus-Auriga is enhanced by a factor of two compared to solar-type stars on the main sequence (Duqennoy & Mayor 1991). Surveys in the Orion Trapezium Cluster found a frequency of binary systems with separations between 60 and 500 AU similar to that of main-sequence stars (e.g. Prosser et al. 1994; Petr et al. 1998). Scally et al. (1999) used proper motion data to search for binaries with separations in the range 1000 -- 5000 AU and got the result that the Orion cluster contains no binaries at all in this separation range. Therefore, it is not possible that all main-sequence field stars formed in regions like Taurus-Auriga or the Trapezium Cluster, but a combination of both can explain the period distribution of main-sequence binaries, at least in the range covered by the surveys in Taurus-Auriga and Orion. However, we know that a significant fraction of stars form in OB Associations, which have not been included in this combination. Furthermore, it is not yet clear if the high multiplicity in Taurus-Auriga is typical for T Associations. We will review the binary frequency and period distribution in several star forming regions and discuss the implications for the origin of the field star population.
Koehler Rainer
Leinert Ch.
Zinnecker Hans
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