Astronomy and Astrophysics – Astrophysics
Scientific paper
2008-07-30
EAS Publication Series 29, 2008
Astronomy and Astrophysics
Astrophysics
24 pages, 11 figures, lecture notes of "Stellar Physics Summer School 2005", on "Tidal effects in stars, planets and disks"
Scientific paper
10.1051/eas:0829002
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.
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