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- W2040474514 abstract "A linearized formalism is presented for the calculation of the tidally produced gravitational radiation potential h/sup TT/ from binary systems with arbitrary orbits. The stars are Newtonian, isentropic, and nonrotating. Normal-mode analysis is used to calculate the tidally generated internal motions; the resulting radiation potential h/sup TT/ and its Fourier decomposition are calculated in the Newtonian limit of the multipole formalism. The tidal radiation potential is weaker than that produced by the orbital motion by a factor of order ((stellar radius)/(periastron distance))/sup 5/. If we assume that the time scale of the tidal perturbation is always much less than the damping time of the star, then if in addition the damping time is much less than the time between periastron passages, the radiation spectrum consists of the l=2 eigenfrequencies of the star near the fundamental l=2 eigenfrequency; if the reverse is true (damping time >> time between periastrons), the spectrum is similar to the orbital gravitational radiation specturm." @default.
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- W2040474514 date "1977-09-01" @default.
- W2040474514 modified "2023-09-26" @default.
- W2040474514 title "Tidal generation of gravitational waves from orbiting Newtonian stars. I - General formalism" @default.
- W2040474514 doi "https://doi.org/10.1086/155536" @default.
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