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Seismic Tests of Theoretical Models of HR 1217

Published online by Cambridge University Press:  12 April 2016

M.S. Cunha ,
J.M.M.B. Fernandes  and
M.J.P.F.G. Monteiro
M.S. Cunha
Affiliation:
Centro de Astrofísica da Universidade do Porto, Portugal Instituto Superior da Maia, Portugal
J.M.M.B. Fernandes
Affiliation:
Observatorio Astronómico da Universidade de Coimbra, Portugal
M.J.P.F.G. Monteiro
Affiliation:
Centro de Astrofísica da Universidade do Porto, Portugal Departamento de Matemática Aplicada da Faculdade de Ciencias, Universidade do Porto, Portugal

Extract

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A way in which we might learn about the physics of the interior of roAp stars is by studying their oscillations. To that aim we have initiated a study in order to investigate what additional constraints might be imposed to the physics of the interior of roAp stars from the study of their oscillation spectra. We have chosen to start this work by studying the well known multi-periodic roAp star HR 1217. The observed data used for HR1217 were L/L⊙=7.8±0.7 and Teff=7400±100 K, from Matthews et al. (1999), Zs=0.009 estimated from Ryabchikova et al. (1997), and Δv=67.91±0.12μHz from Kurtz et al. (1989).

Type
Part 2.3. Chemically Peculiar Stars
Information
International Astronomical Union Colloquium , Volume 185: Radial and Nonradial Pulsations as Probes of Stellar Physics , 2002 , pp. 302 - 303
Copyright
Copyright © Astronomical Society of the Pacific 2002

References

Cunha, M.S., Fernandes, J.M.M.B., Monteiro, M.J.P.F.G. 2001, in ASP Conf. Ser., Observed HR Diagrams and Stellar Evolution, eds. Fernandes, J. & Lejeune, T., (San Francisco ASP), in pressGoogle Scholar
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