Multi-site photometry of the pulsating Herbig Ae star V346 Ori*
INAF – Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy e-mail: firstname.lastname@example.org
2 Departimento de Astrofísica, Universidad de La Laguna, Avda. Astrofisico F. Sánchez sn, 30071 La Laguna, Spain
3 INAF – Osservatorio Astronomico di Capodimonte, via Moiariello 16, 80131 Napoli, Italy e-mail: [ripepi;marconi]@oacn.inaf.it, [ruoppo;leccia]@oacn.inaf.it
4 DMA – Faculdade de Ciências and Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal e-mail: Mario.Monteiro@astro.up.pt
5 Instituto de Astrofísica de Andalucía, CSIC, Apdo. 3004, 18080 Granada, Spain e-mail: [eloy;pja;fja;mjlg]@iaa.es
6 Florida Institute of Technology, Department of Physics and Space Science, 150 W Univ. Blvd., Melbourne, FL 32901-6988, USA e-mail: email@example.com
7 INAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy e-mail: firstname.lastname@example.org
8 INAF – Osservatorio Astrofisico di Catania, via S. Sofia 78, 95123 Catania, Italy e-mail: email@example.com
Accepted: 21 March 2009
Context. The study of pulsation in pre-main-sequence intermediate-mass stars represents an important tool for deriving information about fundamental stellar parameters and internal structure, as well as testing theoretical models. Interest in this class of variable stars has increased significantly during the last decade and about 30 members are presently known in the literature.
Aims. After constructing the frequency spectrum of oscillations in V346 Ori, we apply asteroseismic tools to these data to estimate the intrinsic parameters (mass, luminosity, effective temperature) of V346 Ori and obtain information about its internal structure.
Methods. CCD time-series photometry in the Johnson V filter was obtained for a total of 145.7 h of observations distributed over 36 nights. The resulting light curves were subjected to a detailed frequency analysis using updated numerical techniques. Photometric and spectroscopic data were also acquired to determine reliable estimates of the stellar properties.
Results. We identified 13 oscillation frequencies, 6 of which with higher significance. These were compared with the predictions of non-radial adiabatic models. The resulting best-fit model corresponds to a mass of , luminosity , and effective temperature K. These values are marginally consistent with the association of V346 Ori to Orion OB1a. Alternatively, V346 Ori could be placed at a slightly larger distance than previously estimated.
Key words: stars: pre-main sequence / stars: oscillations / stars: individual V346 Orionis / stars: fundamental parameters
© ESO, 2009