Abstract
High-resolution echelle spectra have been obtained for low-mass pre-main-sequence stars in the Taurus-Auriga, Orion, Chamaeleon, Ophiuchus, and other star formation regions. Using temperature-sensitive individual metallic ratios, new effective temperatures are determined for a sample of 30 G and K pre-main-sequence stars in nearby star-forming clouds to an accuracy of ± 200 K or better in most cases. Comparison of these values with previous spectral classifications using low-resolution spectra reveals occasional large discrepancies in spectral type. Microturbulences derived for 23 weak line T Tauri stars range as high as 3.1 ± 0.4 km s–1. The mean microturbulent velocity of the sample is 1.6 ± 0.6 km s–1. Using these new effective temperatures and microturbulences, iron abundances have been determined for 30 pre-main-sequence stars in several northern and southern sky star-formation regions. By determining the mean [Fe/H] for at least five stars in each cloud, bulk metallicities have been derived for the Taurus-Auriga, Orion, Chamaeleon, and Ophiuchus molecular clouds. [Fe/H] is approximately solar in all the regions surveyed.
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