Dynamical tide in solar-type binaries

Jeremy Goodman, Eric S. Dickson

Research output: Contribution to journalArticlepeer-review

128 Scopus citations


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
Issue number2 PART I
StatePublished - 1998

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science


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


Dive into the research topics of 'Dynamical tide in solar-type binaries'. Together they form a unique fingerprint.

Cite this