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| Paper: |
Physical Mechanisms for Tidal Dissipation |
| Volume: |
333, Tidal Evolution and Oscillations in Binary Stars: Third Granada Workshop on Stellar Structure |
| Page: |
4 |
| Authors: |
Zahn, J.-P. |
| Abstract: |
A binary system tends to its state of minimum kinetic energy, for given (and conserved) angular momentum : circular orbit, all spins aligned, and rotation of the components synchronized with the orbital motion. The pace at which this final state is achieved depends on the physical processes which are responsible for the dissipation of the 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. I shall review these physical processes, discuss the uncertainties of their present treatment, present the latest developments, and compare the theoretical predictions with the observed properties concerning the orbital circularization of close binaries. |
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