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New Observations of the Pulsating PMS Star V351 Ori

  • M. Marconi (a1), V. Ripepi (a1), S. Bernabei (a2) and F. Palla (a3)

Abstract

We present new photoelectric observations of the Pre–Main-Sequence δ Scuti star, V351 Ori. These new data suggest that V351 Ori could be a multiperiodic variable. The comparison between observations and detailed pulsational models allows us to put 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 M 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.

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Copyright

References

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Marconi, M. & Palla, F. 1998, ApJ, 507, L141
Marconi, M., Ripepi, V, Bernabei, S., Palla, F., Alcalá, J.M., Covino, E., & Terranegra, L. 2001, A&A, 372, L21 (M01)

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