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New Observations of the Pulsating PMS Star V351 Ori

Published online by Cambridge University Press:  12 April 2016

M. Marconi ,
V. Ripepi ,
S. Bernabei  and
F. Palla
M. Marconi
Affiliation:
Osservatorio Astronomico di Capodimonte, Italy
V. Ripepi
Affiliation:
Osservatorio Astronomico di Capodimonte, Italy
S. Bernabei
Affiliation:
Osservatorio Astronomico di Bologna, Italy
F. Palla
Affiliation:
Osservatorio Astronomico di Arcetri, Italy

Abstract

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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.

Type
Part 2.4. Delta Scuti Stars
Information
International Astronomical Union Colloquium , Volume 185: Radial and Nonradial Pulsations as Probes of Stellar Physics , 2002 , pp. 348 - 349
Copyright
Copyright © Astronomical Society of the Pacific 2002

References

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