Quasiperiodic oscillations around hairy black holes in Horndeski gravity

TL;DR

This paper investigates the motion of test particles and quasiperiodic oscillations around non-rotating hairy black holes in Horndeski gravity, analyzing frequency models, orbit behaviors, and astrophysical implications for microquasars.

Contribution

It provides a detailed analysis of QPO frequencies and orbit behaviors in Horndeski gravity, including constraints on the Horndeski parameter and black hole mass estimates.

Findings

QPO frequencies depend on the Horndeski parameter q.

ISCO radius reaches 6M at a critical q value, matching Schwarzschild case.

QPO orbit locations are close to the ISCO, within observational errors.

Abstract

Testing gravity theories and their parameters using observations is an important issue in relativistic astrophysics. In this context, we investigate the motion of test particles and their harmonic oscillations in the spacetime of non-rotating hairy black holes (BHs) in Hordeski gravity, together with astrophysical applications of quasiperiodic oscillations (QPOs). We show possible values of upper and lower frequencies of twin-peak QPOs which may occur in the orbits from innermost stable circular orbits to infinity for various values of the Horndeski parameter $q$ in relativistic precession, warped disk models, and three different sub-models of the epicyclic resonant model. We also study the behaviour of the QPO orbits and their position relative to innermost stable circular orbits (ISCOs) with respect to different values of the parameter $q$. {It is obtained that at a critical value of the Horndeski parameter ISCO radius takes $6M$ which has been in the pure Schwarzschild case.} Finally, we obtain mass constraints of the central BH of microquasars GRS 1915+105 and XTE 1550-564 at the GR limit and the possible value of the Horndeski parameter in the frame of the above-mentioned QPO models. The analysis of orbits of twin peak QPOs with the ratio of upper and lower frequencies 3:2, around the BHs in the frame of relativistic precession (RP) and epicyclic resonance (ER4) QPO models have shown that the orbits locate close to the ISCO. The distance between QPO orbits and ISCO is obtained to be less than the error of the observations.