| Issue |
A&A
Volume 408, Number 3, September IV 2003
|
|
|---|---|---|
| Page(s) | 1047 - 1055 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361:20031011 | |
| Published online | 17 November 2003 | |
Multisite observations of the PMS δ Scuti star V351 Ori *,**
1
INAF-Osservatorio Astronomico di Capodimonte, Via Moiariello 16, 80131 Napoli, Italy
2
INAF-Osservatorio Astronomico di Bologna, Via Ranzani 1, 40127 Bologna, Italy
3
Departimento de Astrofísica, Universidad de La Laguna, Avda. Astrofisico F. Sánchez sn, 30071 La Laguna, Spain
4
INAF-Osservatorio Astrofisico di Arcetri, Largo E. Fermi, 5, 50125 Firenze, Italy
5
Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
6
Florida Inst. Technology, 150 W Univ. Blvd., Melbourne, FL 32901-6988, USA
7
Instituto de Astronomía, UNAM, Apdo. Postal 70-264, México D.F., CP 04510, México
8
National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100012, PR China
Corresponding author: V. Ripepi, ripepi@na.astro.it
Received:
5
September
2002
Accepted:
20
June
2003
We present the results of multisite observations
spanning two years on the pre–main-sequence (PMS) star V351 Ori.
A total of around 180 hours of observations over 29 nights have been
collected, allowing us to measure five different periodicities,
most likely related to the δ Scuti variability of V351 Ori.
Comparison with the predictions of linear
nonadiabatic radial pulsation models put stringent constraints on the
stellar parameters and
indicate that the distance
to V351 Ori is intermediate between the lower limit measured by Hipparcos
(210 pc)
and that of the Orion Nebula (450 pc). However, radial pulsation models are
unable to reproduce all of the observed frequencies with a single choice
of (
, 
, and Teff), suggesting
the presence of additional nonradial modes.
Key words: stars: variables: δ Scuti / stars: oscillations / stars: pre-main sequence / stars: fundamental parameters / stars: individual: V351 Ori
Based on observations collected at the: Loiano Observatory (Italy), San Pedro Martir Observatory (México), OGS at Teide Observatory (Spain), JKT at Roque de los muchachos Observatory (Spain), Beijing Astronomical Observatory (China), SARA Observatory at Kitt Peak, which is owned and operated by the Southeastern Association for Research in Astronomy.
© ESO, 2003
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