Rotational evolution of Post-T Tauri stars in Lindroos binary systems

Details Rotational evolution of Post-T Tauri stars in Lindroos binary systems Rotational evolution of Post-T Tauri stars in Lindroos binary systems

Aug 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000noao.prop..235w&link_type=abstract

NOAO Proposal ID #2000B-0235

Computer Science

Scientific paper

We proposed UBVRI photometric observations of the first unbiased and reliable sample of Post-T Tauri stars (PTTS) in order to derive their ages and rotational periods. Previous studies fail in deriving the rotational properties of PTTS because (i) the samples were not reliable due to uncertainties in the age determination of the PMS objects and (ii) the samples were selected according to the X-ray detection of the sources, so they were always biased towards fast rotators. However, we select our sample in an indirect way, studying binary systems comprised of a young Main Sequence (MS) early-type star (ages ~ 10 -150 Myr) and a late-type (F,G,K and M) secondary, the so-called Lindroos binary systems. If the systems are bound, the secondaries are late-type stars with similar ages to the primaries (~10^7yr), that is, PTTS. The presence of the Li I (6708Å) absorption line and the Ca II (H & K) in the spectra of the secondaries, as well as their X-ray detection confirms these stars as a reliable sample of PTTS. The wide range of X- ray luminosities reported in these stars suggests different rotational properties among the sample, that is, it is an unbiased sample that includes slow and fast rotators. Therefore, this is an appropriate sample to understand the evolution of PMS late-type stars as they contract to the MS.

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