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GR: Fachverband Gravitation, Relativistische Astrophysik und Kosmologie

GR 3: Classical General Relativity I

GR 3.5: Talk

Monday, March 16, 2026, 17:15–17:30, KH 02.012

Relativistic orbital perturbation theory — Oleksii Yanchyshen, Eva Hackmann, and •Claus Lämmerzahl — ZARM and ITP, University of Bremen

Within a Newtonian framework orbital perturbation theory is based on the Keplerian orbits as exact solution of the Kepler problem. Perturbation forces lead to time dependent orbital parameters like the semimajor axis, eccentricity, inclination, perigee, and ascending node. Within a relativistic framework we start with the exact solution of the geodesic equation in Schwarzschild space-time. Perturbation forces then lead to a time-dependence of orbital parameters, some of which we newly defined. Their time dependence is described by a relativistic generalization of the Gauß equations. In the presentation this formalism is explained and some applications to perturbations like radiation reaction will be outlined. This new approach is mathematically more challenging but leads to a faster convergence of results than post-Newtonian approaches in the strong field regime.