Relativistic canonical planetary perturbation equations for momentum‐dependent forces, and the Lense‐Thirring precession

Relativistic planetary perturbation theory based on canonical equations of motion, rather than on the use of osculating orbital elements, is developed and applied to two problems. Differences between the canonical form of perturbation theory and the classical Lagrange planetary perturbation equations are discussed. The canonical form of perturbation theory in some cases has advantages when the perturbing forces are momentum‐dependent, but the two forms of perturbation theory are equivalent if the perturbing forces are dependent only on position and not on momentum. The canonical form of the planetary perturbation equations are derived and applied to the Lense‐Thirring precession of a test body in a Keplerian orbit around a rotating mass source.