Extrasolar planetary dynamics with a generalized planar Laplace-Lagrange secular theory

Details Extrasolar planetary dynamics with a generalized planar Laplace-Lagrange secular theory Extrasolar planetary dynamics with a generalized planar Laplace-Lagrange secular theory

2007-03-05

arxiv.org/abs/astro-ph/0703088v1

Astrophys.J.661:1311-1322,2007

Astronomy and Astrophysics

Astrophysics

14 pages, 12 figures, 1 table, accepted for publication in ApJ

Scientific paper

10.1086/516726

The dynamical evolution of nearly half of the known extrasolar planets in multiple-planet systems may be dominated by secular perturbations. The commonly high eccentricities of the planetary orbits calls into question the utility of the traditional Laplace-Lagrange (LL) secular theory in analyses of the motion. We analytically generalize this theory to fourth-order in the eccentricities, compare the result with the second-order theory and octupole-level theory, and apply these theories to the likely secularly-dominated HD 12661, HD 168443, HD 38529 and Ups And multi-planet systems. The fourth-order scheme yields a multiply-branched criterion for maintaining apsidal libration, and implies that the apsidal rate of a small body is a function of its initial eccentricity, dependencies which are absent from the traditional theory. Numerical results indicate that the primary difference the second and fourth-order theories reveal is an alteration in secular periodicities, and to a smaller extent amplitudes of the planetary eccentricity variation. Comparison with numerical integrations indicates that the improvement afforded by the fourth-order theory over the second-order theory sometimes dwarfs the improvement needed to reproduce the actual dynamical evolution. We conclude that LL secular theory, to any order, generally represents a poor barometer for predicting secular dynamics in extrasolar planetary systems, but does embody a useful tool for extracting an accurate long-term dynamical description of systems with small bodies and/or near-circular orbits.

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