The dynamical tide in close binaries

Details The dynamical tide in close binaries The dynamical tide in close binaries

Jul 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975a%26a....41..329z&link_type=abstract

Astronomy and Astrophysics, vol. 41, no. 3-4, July 1975, p. 329-344.

Astronomy and Astrophysics

Astrophysics

196

Asymptotic Methods, Binary Stars, Gravitational Effects, Stellar Structure, Tides, Radiative Transfer, Stellar Envelopes, Stellar Gravitation, Stellar Rotation

Scientific paper

The non-adiabatic oscillations of a star, driven by an outer rotating gravitational field, have been studied by the use of matched asymptotic expansions. The interior and envelope solutions in this procedure are derived in Sections 2 and 3. The results apply to stars which have a convective core and a radiative envelope, and they are discussed in Section 4. We find that the resonances of the free gravity modes are damped by radiative dissipation, which operates in a relatively thin region below the surface of the star. Due to that dissipation, some properties of the dynamical tide have observable consequences in close binary systems: (1) A torque is applied to a binary component; this serves to make it corotate with its companion in a time which can be short compared to its nuclear life. (2) Before that synchronization is achieved, the brightness distribution over the surface of the star is in general phase shifted relative to the external driving potential.

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