2008/01/01 by Jean-Paul Zahn, J.-P. Zahn · 5 citations
Engineering · Physics and Astronomy · #Fluid dynamics and aerodynamics studies #Solar and Space Plasma Dynamics #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1051/eas:0829002
published as EAS Publication Series 29, 2008 · 24 pages, 11 figures, lecture notes of "Stellar Physics Summer School 2005", on "Tidal effects in stars, planets and disks"
openalex publication_date 2008/01/01 · arxiv created 2008/07/30 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/31
To first approximation, a binary system conserves its angular momentum while it evolves to its state of minimum kinetic energy: circular orbit, all spins aligned, and components rotating in synchronism with the orbital motion. The pace at which this final state is achieved depends on the physical processes that are responsible for the dissipation of the tidal kinetic energy. For stars (or planets) with an outer convection zone, the dominant mechanism identified so far is the viscous dissipation acting on the equilibrium tide. For stars with an outer radiation zone, it is the radiative damping operating on the dynamical tide. After a brief presentation of the tides, I shall review these physical processes; I shall discuss the uncertainties of their present treatment, describe the latest developments, and compare the theoretical predictions with the observed properties concerning the orbital circularization of close binaries.