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An Improved Method of Photometric Mode Identification: Applications to Slowly Pulsating B, β Cephei, δ Scuti and γ Doradus Stars

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Abstract

We present an improved version of the method of photometric mode identification based upon the inclusion of non-adiabatic eigenfunctions determined in the stellar atmosphere, according to the formalism recently proposed by Dupret et al. (2002).We apply our method to β Cephei, Slowly Pulsating B, δ Scuti and γ Doradus stars. Besides identifying the degree ℓ of the pulsatingstars, our method is also a tool for improving the knowledge of stellar interiors and atmospheres, by imposing constraints on the metallicity for β Cephei and SPBs, the characteristics of the superficial convection zone for δ Scuti and γ Doradus starsand the limb-darkening law.

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Authors and Affiliations

  1. Institut d'Astrophysique et de Géophysique de, l'Université de Liège, Belgium

    M.-A. Dupret, R. Scuflaire, A. Noels & A. Thoul

  2. Instituto de Astrofí sica de Andalucía-CSIC, Granada, Spain

    R. Garrido & A. Moya

  3. Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Belgium

    J. De Ridder, P. De Cat & C. Aerts

Authors
  1. M.-A. Dupret
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  2. R. Scuflaire
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  3. A. Noels
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  4. A. Thoul
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  5. R. Garrido
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  6. A. Moya
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  7. J. De Ridder
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  8. P. De Cat
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  9. C. Aerts
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Dupret, MA., Scuflaire, R., Noels, A. et al. An Improved Method of Photometric Mode Identification: Applications to Slowly Pulsating B, β Cephei, δ Scuti and γ Doradus Stars. Astrophysics and Space Science 284, 129–132 (2003). https://doi.org/10.1023/A:1023262813348

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  • DOI: https://doi.org/10.1023/A:1023262813348

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