Spin Interaction under the Collision of Two Kerr-(anti-)de Sitter Black Holes

TL;DR

This paper explores how spin interactions between colliding Kerr-(anti-)de Sitter black holes influence gravitational radiation, highlighting the dependence on black hole rotation directions, cosmological constant, and stability, with thermodynamic bounds providing insights.

Contribution

It introduces an analysis of spin interaction effects on gravitational radiation during black hole collisions, considering the influence of the cosmological constant and stability, which is a novel approach.

Findings

Spin interaction potential depends on the relative rotation directions.

Gravitational radiation is influenced by the cosmological constant.

Thermodynamic bounds estimate the upper limits of radiation.

Abstract

We have investigated spin interaction under the collision of Kerr-(anti-)de Sitter black holes. The potential of a spin interaction is dependent on the relative rotating directions of the black holes, and this potential can be released as gravitational radiation under the collision. The radiation depends on the cosmological constant and corresponds to the potential of the spin interaction at a limit where one of the black holes is assumed to have small mass and angular momentum. Then, we have shown, approximately, the overall behaviors of the upper bounds on the radiation using thermodynamics. From these bounds, the spin interaction can consistently contribute to the radiation. In addition, the radiation depends on the stability of the black hole synthesized from the collision.