SpringerLink
Forum Springer Astron. Astrophys.
Forum Whats New Search Orders


Astron. Astrophys. 342, 173-178 (1999)

Next Section Table of Contents

On the evolutionary status of X-ray selected weak-line T Tauri star candidates in Taurus-Auriga *

E.L. Martín 1,2 and A. Magazzù 3,4

1 University of California, 601 Campbell Hall, Berkeley, CA 94720, USA
2 Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain
3 Centro Galileo Galilei, Apartado 565, E-38700 Santa Cruz de La Palma, Spain
4 Osservatorio Astrofisico di Catania, Cittá Universitaria, I-95125 Catania, Italy

Received 13 May 1998 / Accepted 3 November 1998

Abstract

We present lithium observations of 35 stars previously reported by Wichmann et al. (1996) to be possible new weak T Tauri stars (WTTS) discovered by ROSAT in the Taurus-Auriga star-forming region. These stars were identified on the basis of low-resolution optical spectra. We have used our higher resolution spectra for measuring the equivalent widths of the Li I  670.8 nm resonance line, and for revisiting the evolutionary status of these stars. Most ([FORMULA]85%) of the stars in our sample coming from ROSAT pointed observations are indeed confirmed to be new WTTS, but only a minority ([FORMULA]22%) of the stars coming from the ROSAT all-sky survey are confirmed as WTTS. There are two reasons why we reject some stars as WTTS. One is that seven of the stars do not have a detectable lithium line at all. The other is that we use a definition different from that Wichmann et al. (1996) for classifying stars as WTTS. In particular, we identify eight stars as post T Tauri stars (PTTS) on the basis of their moderate lithium depletion. Our results confirm that the widely dispersed RASS-selected candidate WTTS tend to be older than the T Tauri stars associated with dark molecular clouds. The presence of PTTS around central Taurus suggests that the clouds may have been forming stars for more than [FORMULA]10 Myr, although at a very low rate. On the basis of the PTTS identified in this work we discuss possible differences between them and the WTTS. We find that PTTS seem to have slightly lower H[FORMULA] emission equivalent width than WTTS, but the small number of known PTTS prevent us from making a strong conclusion.

Key words: stars: abundances – stars: activity – stars: pre-main sequence – X-rays: stars

* Based on observations made with the Isaac Newton and the William Herschel telescopes operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias

Send offprint requests to: E.L. Martín (ege@popsicle.berkeley.edu)

SIMBAD Objects

Contents

Next Section Table of Contents

© European Southern Observatory (ESO) 1999

Online publication: December 22, 1998
helpdesk.link@springer.de