EDP Sciences
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Volume 378, Number 3, November II 2001
Page(s) 1003 - 1013
Section Formation, structure and evolution of stars
DOI http://dx.doi.org/10.1051/0004-6361:20011285

A&A 378, 1003-1013 (2001)
DOI: 10.1051/0004-6361:20011285

Infall variability in the Classical T Tauri system VZ Chamaeleonis

K. Smith1, 2, G. F. Lewis3, I. A. Bonnell4 and J. P. Emerson5

1  Institut für Astronomie, ETH-Zentrum, 8092 Zürich, Switzerland
2  Paul Scherrer Institut, Würenlingen und Villigen, 5232 Villigen PSI, Switzerland
3  Anglo-Australian Observatory, PO Box 296, Epping, NSW 1710, Australia
    e-mail: gfl@aaoepp.aao.GOV.AU
4  University of St Andrews, St Andrews, Scotland
    e-mail: iab1@st-andrews.ac.uk
5  Department of Physics, Queen Mary, University of London, Mile End Road, London E1 4NS, UK
    e-mail: j.p.emerson@qmw.ac.uk

(Received 11 June 2001 / Accepted 13 September 2001)

We present time series spectroscopy of the Classical T Tauri star VZ Cha. We follow spectral variations at intermediate resolution over five successive nights, or approximately two rotation periods. We see profile features which persist on timescales longer than the expected infall time from the inner disc, and we see expected evidence of rotational variations in the lines, but we also note that rotation alone cannot produce all the observed variability and some other mechanism must be invoked. The behaviour of H$\alpha$ is observed to be markedly different from that of the other lines. In particular, the evidence of rotational effects is lacking at H$\alpha$, and the activity in the red and blue wings of the line is not significantly correlated, in contrast to the other Balmer lines.

Key words: accretion -- accretion disks -- stars: activity, pre-main sequence, variables: general

Offprint request: K. Smith, kester@astro.phys.ethz.ch

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