Periodic radial velocity variations in RU Lupi

¹ School of Physics & Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS, Scotland, UK e-mail: Eric.Stempels@st-andrews.ac.uk
² Stockholm Observatory, AlbaNova University Centre, 106 91 Stockholm, Sweden
³ Crimean Astrophysical Observatory, p/o Nauchny, Crimea 98409, Ukraine

Received: 24 March 2006
Accepted: 15 September 2006

Abstract

Context. RU Lup is a Classical T Tauri star with unusually strong emission lines, which has been interpreted as manifestations of accretion. Recently, evidence has accumulated that this star might have a variable radial velocity.

Aims.We intended to investigate in more detail the possible variability in radial velocity using a set of 68 high-resolution spectra taken at the VLT (UVES), the AAT (UCLES) and the CTIO (echelle).

Methods.Using standard cross-correlation techniques, we determined the radial velocity of RU Lup. We analysed these results with Phase-dispersion minimization and the Lomb-Scargle periodogram and searched for possible periodicities in the obtained radial velocities. We also analysed changes in the absorption line shapes and the photometric variability of RU Lup.

Results.Our analysis indicated that RU Lup exhibits variations in radial velocity with a periodicity of 3.71 days and an amplitude of 2.17 km s^-1. These variations can be explained by the presence of large spots, or groups of spots, on the surface of RU Lup. We also considered a low-mass companion and stellar pulsations as alternative sources for these variations but found these to be unlikely.