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The seismology of sun-like stars

  • P. Demarque
  • D. B. Guenther
Part VI Seismology of Stars
Part of the Lecture Notes in Physics book series (LNP, volume 367)

Abstract

By observing the p-mode oscillation spectrum of a star and determining its first and second order frequency spacings, Δv and δ, it is possible to obtain constraints which are useful in modeling the star. We show, as an example, how the positions of the frequencies of the p-modes changes from the familiar “picket fence” or regular spacing to a more random irregular spacing as the sun evolves from the ZAMS to the base of the giant branch. For α Cen, ε Eri, Procyon, Arcturus, and μ Cas we describe, in specific terms, how the frequency spacings can be used to improve our knowledge about each of these stars. We discuss the important advantages of observing the p-modes of stars in star clusters. We also discuss how rotational splittings could be used along with other stellar diagnostics to infer the rotational history of the star's interior.

Keywords

White Dwarf Convection Zone Helium Abundance Halo Star Picket Fence 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© Springer-Verlag 1990

Authors and Affiliations

  • P. Demarque
    • 1
  • D. B. Guenther
    • 1
  1. 1.Center for Solar and Space ResearchYale UniversityNew HavenU.S.A.

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