POSTER PAPER 3.08
The Short-period Multiplicity Among the T-Tauri Stars
C.H.F. Melo
Institute: Observatoire de Geneve
Contact Email: cmelo@eso.org
Abstract:
We present in this paper the results of high-resolution spectroscopic observations carried out
during three years aiming to estimate the short-period (Porb < 100 days) binary frequency of a
sample of T-Tauri stars in Oph-Sco, Cha, Lup, CrA star forming regions (SFRs) already observed
with high angular resolution techniques by Ghez et al. (1993) and by Ghez et al. (1997) to detect
more wider components. When combining all four SFRs, the short-period binary frequency is
indistinguishable of that found by Duquennoy & Mayor (1991) for the solar-type field stars which
is also consistent with the previous result obtained by Mathieu (1992, 1994). When Oph-Sco is
analyzed separately, it seems that there is an excess of short-period binaries of a factor 2-2.5,
on the opposite, short-period binary systems seem to be absent in the sample containing stars in
Cha/Lup/CrA. Such a trend was equally found by Mathieu (1992). However, the small size of the
sample avoid drawing any robust conclusion about a possible excess (lack) of short-period binaries
in Oph (Cha/Lup/CrA).
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Manuscript submitted: 2001-Sep-06
"The Future of Cool-Star Astrophysics", 2003, Eds. A. Brown,
G. M. Harper, & T. R. Ayres.
Proceedings of 12th Cambridge Workshop on Cool Stars, Stellar Systems,
& The Sun,
© 2003 University of Colorado.