Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984a%26a...141..232s&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 141, no. 1, Dec. 1984, p. 232-240.
Astronomy and Astrophysics
Astrophysics
27
Celestial Mechanics, Gravitational Effects, Stellar Motions, Three Body Problem, Triple Stars, Binary Stars, Deformation, Eccentricity, Hamiltonian Functions, Numerical Integration, Tides
Scientific paper
A stable three-body system is characterized by two orbital periods P1 and P2. For P2/P1 greater than some 50:1, the point-mass problem has a well-known second-order analytical solution. It is shown how this solution can be modified to take tidal deformation into account. As expected, the motion becomes qualitatively different when the apsidal advance due to deformation becomes larger than that due to the third body. In particular, there is no longer a "critical" relative inclination, and circular close orbits are allowed at all inclinations. For large period-ratios, even a small deformation may have this effect. For small period-ratios, the previously neglected third-order terms become important. The tidal forces have important evolutionary consequences and as a first step towards better understading, a "classification" of triple stars is introduced.
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