Dynamical tide in solar-type binaries

Jeremy Goodman, Eric S. Dickson

    Research output: Contribution to journalArticle

    Abstract

    Circularization of late-type main-sequence binaries is usually attributed to turbulent convection, while that of early-type binaries is explained by resonant excitation of gr-modes. We show that the latter mechanism also operates in solar-type stars and is at least as effective as convection despite inefficient damping of g-modes in the radiative core. The maximum period at which this mechanism can circularize a binary composed of solar-type stars in 1010 yr is as low as 3 days, if the modes are damped by radiative diffusion only and g-mode resonances are fixed, or as high as 6 days if one allows for evolution of the resonances and for nonlinear damping near inner turning points. Even the larger theoretical period falls short of the observed transition period by a factor of 2.

    Original languageEnglish (US)
    Pages (from-to)938-944
    Number of pages7
    JournalAstrophysical Journal
    Volume507
    Issue number2 PART I
    DOIs
    StatePublished - 1998

    Keywords

    • Binaries: close
    • Binaries: spectroscopic
    • Stars: interiors
    • Stars: oscillations

    ASJC Scopus subject areas

    • Astronomy and Astrophysics
    • Space and Planetary Science

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    Goodman, J., & Dickson, E. S. (1998). Dynamical tide in solar-type binaries. Astrophysical Journal, 507(2 PART I), 938-944. https://doi.org/10.1086/306348