Geodetic Motion Around Rotating Blackhole in Nonlocal Gravity

TL;DR

This paper investigates the properties of rotating black holes in a non-local gravity model, deriving metrics and orbital frequency shifts to assess the theory's strong field predictions and potential observational signatures.

Contribution

It derives Kerr-like metrics and orbital frequency shifts for black holes in a non-local gravity model, advancing the understanding of strong field tests in modified gravity theories.

Findings

Derived Kerr-like black hole metric in non-local gravity

Calculated orbital frequency shifts for test particles

Provided weak gravity regime metric for rotating objects

Abstract

Recently the non-local gravity theory has come out to be a good candidate for an effective field theory of quantum gravity and also it can provide rich phenomenology to understand late-time accelerating expansion of the universe. For any valid theory of gravity, it has to surmount solar system tests as well as strong field tests. Having motivations to prepare the framework for the strong field test of the modified gravity using Extreme Mass Ratio Inspirals(EMRIs), here we try to obtain the metric for Kerr-like blackhole for a non-local gravity model known as RR model and calculate the shift in orbital frequencies of a test particle moving around the blackhole. We also derive the metric for a rotating object in the weak gravity regime for the same model.