The authors present the results of a study of five X-ray discovered weak emission pre-main-sequence stars in the Taurus-Auriga star formation complex. All are of spectral type K7-M0, and about 1-2 mag above the main sequence. One is a double-lined spectroscopic binary, the first spectroscopic binary PMS star to be confirmed. The ages, masses, and radii of these stars as determined by photometry and spectroscopy are discussed. The authors investigate the difference in emission strength between these and the T Tauri stars and conclude that these "post-T Tauri" stars do indeed appear more evolved than the T Tauri stars, although there is no evidence of any significant difference in ages.
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Mundt et al. (1983) studied this question.