Observations of suspected low-mass post-T tauri stars and their evolutionary status

Journal Article · Wed Jun 01 04:00:00 EDT 1983 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/161033· OSTI ID:5600385

Mundt, R; Walter, F M; Feigelson, E D; Finkenzeller, U; Herbig, G H; Odell, A P

We present the results 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. We discuss the ages, masses, and radii of these stars as determined by photometry and spectroscopy. We 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.

• Research Organization: Steward Observatory, University of Arizona
• OSTI ID: 5600385
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 269:1; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
BINARY STARS
COSMIC RAY SOURCES
COSMIC X-RAY SOURCES
ERUPTIVE VARIABLE STARS
MAIN SEQUENCE STARS
PHOTOMETRY
RADIAL VELOCITY
SPECTROSCOPY
STAR EVOLUTION
STARS
T TAURI STARS
VARIABLE STARS
VELOCITY