New observations of the pulsating PMS star V351 Ori

¹ Osservatorio Astronomico di Capodimonte, Via Moiariello 16, 80131 Napoli, Italy
² Osservatorio Astronomico di Bologna, Via Ranzani 1, 40127 Bologna, Italy
³ Dipartimento de Astrofísica, Universidad de La Laguna, Avda. Astrofisico F. Sànchez sn, 30071 La Laguna, Spain
⁴ Osservatorio Astrofisico di Arcetri, Largo E. Fermi, 5, 50125 Firenze, Italy

Corresponding author: V. Ripepi, ripepi@na.astro.it

Received: 23 March 2001
Accepted: 17 April 2001

Abstract

We present new precise photoelectric observations of the Pre-Main-Sequence δ Scuti star, V351 Ori. These new data show that V351 Ori pulsates in a mixture of several radial modes (at least four). The comparison between observations and detailed pulsational models, allows us to provide independent constraints on the mass and luminosity of the star. The predicted distance is 210 pc, indicating that V351 Ori is much closer than the Orion star forming region. With an inferred mass of ~1.8 and an uncertain evolutionary stage, V351 Ori represents an excellent candidate for future asteroseismological studies that will assess whether it is a young PMS star (~6 Myr) or an evolved object (~1 Gyr) leaving the main-sequence.