Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003cemda..85..269b&link_type=abstract
Celestial Mechanics and Dynamical Astronomy, v. 85, Issue 3, p. 269-291 (2003).
Astronomy and Astrophysics
Astronomy
2
General Relativity, Gravitational Radiation, Restricted Three-Body Problem, Binary Pulsar Systems
Scientific paper
The distinctive feature of the relativistic restricted three-body problem within the c-5 order of accuracy (2½ post-Newtonian approximation) is the presence of the gravitational radiation. To simplify the problem the motion of the massive binary components is assumed to be quasi-circular. In terms of time these orbits have linearly changing radii and quadratically changing phase angles. By substituting this motion into the Newtonian-like equations of motion one gets the quasi-Newtonian restricted quasi-circular three-body problem sufficient to take into account the main indirect perturbations caused by the binary radiation terms. Such problem admits the Lagrange-like quasi-libration solutions and rather simple quasi-circular orbits lying at large distance from the binary.
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