Relativistic Euler's 3-body problem, optical geometry and the golden ratio

Details Relativistic Euler's 3-body problem, optical geometry and the golden ratio Relativistic Euler's 3-body problem, optical geometry and the golden ratio

2009-09-24

arxiv.org/abs/0909.4413v1

Phys.Rev.D80:104036,2009

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

16 pages, 8 figures

Scientific paper

10.1103/PhysRevD.80.104036

A Weyl solution describing two Schwarzschild black holes is considered. We focus on the Z_2 invariant solution, with ADM mass M_{ADM}=2M_K, where M_K is the Komar mass of each black hole. For this solution the set of fixed points of the discrete symmetry is a totally geodesic sub-manifold. The existence and radii of circular photon orbits in this sub-manifold are studied, as functions of the distance 2L between the two black holes. For L-> 0 there are two such orbits, corresponding to r=3M_{ADM} and r=2M_{ADM} in Schwarzschild coordinates. As the distance increases, it is shown that the two photon orbits approach one another and merge when M_K=\varphi L, where \varphi is the golden ratio. Beyond this distance there exist no circular photon orbits. The two null orbits delimit a forbidden band for time-like circular orbits, which is interpreted in terms of optical geometry. For large L, time-like circular orbits are allowed everywhere, as in the analogous Newtonian problem. The analysis is generalised by considering a Z_2 invariant Weyl solution with an array of N black holes and also by charging the black holes, which connects the Weyl solution to a Majumdar-Papapetrou spacetime.

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