Abstract
A new quantitative least-squares method of identifying the spherical harmonic order from the moments of the line profile is presented. The method is applicable to stars in which the projected rotational velocity is of the same order or less than the pulsational amplitude. Together with a previous method which applies only to stars in which the projected rotational velocity exceeds the pulsational amplitude, it is now possible to obtain an objective mode identification and least-squares estimates of the pulsational parameters for any multiperiodic star.
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References
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© 1990 Springer-Verlag
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Balona, L.A. (1990). Mode identification in a slowly rotating star from line profile variations. In: Osaki, Y., Shibahashi, H. (eds) Progress of Seismology of the Sun and Stars. Lecture Notes in Physics, vol 367. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-53091-6_112
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DOI: https://doi.org/10.1007/3-540-53091-6_112
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