# Relativistic Magnetic Reconnection in Kerr Spacetime

## TL;DR

This paper investigates how the curvature of spacetime around rotating black holes affects magnetic reconnection in relativistic plasmas, revealing that black hole rotation and gravity influence the reconnection rate.

## Contribution

It extends the classical Sweet-Parker model to curved spacetime, analyzing reconnection in Kerr black hole environments with new insights on the effects of rotation and gravity.

## Key findings

- Black hole rotation decreases azimuthal reconnection rate.
- Black hole mass gravitational force reduces radial reconnection rate.
- Spacetime curvature significantly impacts magnetic reconnection processes.

## Abstract

The magnetic reconnection process is analyzed for relativistic magnetohydrodynamical plasmas around rotating black holes. A simple generalization of the Sweet-Parker model is used as a first approximation to the problem. The reconnection rate, as well as other important properties of the reconnection layer, have been calculated taking into account the effect of spacetime curvature. Azimuthal and radial current sheet configurations in the equatorial plane of the black hole have been studied, and the case of small black hole rotation rate has been analyzed. For the azimuthal configuration, it is found that the black hole rotation decreases the reconnection rate. On the other hand, in the radial configuration, it is the gravitational force created by the black hole mass that decreases the reconnection rate. These results establish a fundamental interaction between gravity and magnetic reconnection in astrophysical contexts.