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Astron. Astrophys. 359, 181-190 (2000)


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A study of Li-rich stars discovered by ROSAT in Taurus-Auriga *

R. Wichmann 1, G. Torres 2, C.H.F. Melo 3, S. Frink 4,9, S. Allain 5, J. Bouvier 5, J. Krautter 6, E. Covino 7 and R. Neuhäuser 8

1 Hamburger Sternwarte, University of Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany (rwichmann@hs.uni-hamburg.de)
2 Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
3 Observatoire de Geneve, 51, Ch. des Maillettes, 1290 Sauverny, Suisse
4 Astronomisches Rechen-Institut Heidelberg, Mönchhofstrasse 12-14, 69120 Heidelberg, Germany
5 Laboratoire d'Astrophysique, Observatoire de Grenoble, B.P. 53X, 38041 Grenoble Cedex, France
6 Landessternwarte Königstuhl, 69117 Heidelberg, Germany
7 Osservatorio Astronomico di Capodimonte, Via Moiariello 16, 80131 Napoli, Italy
8 Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse 1, 85740 Garching, Germany
9 UC San Diego, Center for Astrophysics and Space Sciences, 9500 Gilman Drive, La Jolla, CA 92093-0424, USA

Received 21 December 1999 / Accepted 2 May 2000

Abstract

In recent years, large numbers of lithium-rich stars were discovered near several nearby star forming regions (SFRs). We present a detailed study of those stars discovered in and near the central region of the Taurus-Auriga T Tauri association, based on high-resolution echelle spectroscopy and proper motion data. We find that about 60 per cent of our sample can be regarded as pre-main sequence (PMS) stars, while the remaining stars likely are foreground zero-age main sequence (ZAMS) stars. We conclude that the PMS stars are likely associated with the Taurus-Auriga SFR, while the ZAMS stars may represent a population of somewhat older Gould Belt stars. The fraction of ZAMS stars in the Taurus-Auriga sample studied in this work is larger than in a similar sample in the Lupus SFR, and we argue that this may be explained by the spatial structure of the Gould Belt and the Sun's location within it.

Key words: stars: kinematics – stars: pre-main sequence – stars: rotation – X-rays: stars – Galaxy: open clusters and associations: individual: Golud Belt

* Based on observations obtained at Observatoire de Haute Provence. Some of the observations reported here were obtained with the Multiple Mirror Telescope, a joint facility of the Smithsonian Institution and the University of Arizona.

Send offprint requests to: R. Wichmann

© European Southern Observatory (ESO) 2000

Online publication: June 30, 2000

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