Geodesic trajectories for binary systems of supermassive black holes (SMB)

TL;DR

This paper models the spacetime and geodesic trajectories of a binary supermassive black hole system using a weak field approximation, revealing orbital characteristics and energy dynamics influenced by black hole rotation.

Contribution

It introduces a novel metric tensor for binary supermassive black holes and analyzes their geodesic trajectories considering black hole rotation effects.

Findings

Orbital perigee at 116.4 AU and apogee at 969.67 AU.

Orbit precession of 77.8 seconds per year.

Energy per orbit is an order of magnitude higher than Newtonian estimates.

Abstract

During this work, it is considered a binary system of supermassive rotating black holes; first, it is employed the concept of weak field limit to develop a metric tensor g that describes the geometry of the spacetime, it introduced an approximation in which the second black hole is coupled to the system through a perturbation tensor f, consequently , it is employed a black hole type Sagittarius A to make the numerical calculations; the negative Ricci scalar curvature states that the tensor f does not change the topological properties of Kerr solution. From the metric tensor developed and the scalar of curvature the geodesic trajectories are derived; they determine an orbit with a perigee of 116.4AU and an apogee of 969.67AU, the orbit has a precession of 77.8 seconds per year; and the precession is determined by the rotation of the black holes besides the angular momentum that is the classical parametrization; finally, the average energy is defined by the equation E, this expression parametrizes the energy per orbit in function of the rotation of the black holes, this value is one order of magnitude higher than Newtonian energy