Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aspc..333....4z&link_type=abstract
Tidal Evolution and Oscillations in Binary Stars: Third Granada Workshop on Stellar Structure, ASP Conference Series, Vol. 333,
Astronomy and Astrophysics
Astronomy
11
Scientific paper
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.
No associations
LandOfFree
Physical mechanisms for tidal dissipation does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Physical mechanisms for tidal dissipation, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Physical mechanisms for tidal dissipation will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1835396