Thermodynamic properties of the Kerr Black-hole in non-linear electrodynamics with cosmological constant

TL;DR

This paper investigates the thermodynamic properties and horizon structure of slowly rotating Kerr black holes within nonlinear electrodynamics and a cosmological constant, revealing significant modifications to their internal and thermodynamic characteristics.

Contribution

It provides a detailed analysis of how nonlinear electrodynamics and cosmological constant influence Kerr black hole thermodynamics and horizon structure, including mass profiles and parameter space constraints.

Findings

Mass profile $M(r)$ attains a plateau near the cosmological length scale.

Horizon structure depends on rotation parameter $a$, cosmological length $L$, and mass profile.

Thermodynamic parameters $T$, $ abla_h$, and $S$ are computed at horizon surfaces.

Abstract

We study thermodynamic properties, in particular the Temperature~(T), Angular velocity~($\Omega_h$) and Entropy~(S) of the of magnetically charged slowly rotating (with rotation parameter $a \lsim 0.10$) Kerr black-hole(BH) with the inclusion of cosmological constant ($\Lambda$) in the background of nonlinear electrodynamics (NLED). At first we calculated the nonlinear electromagnetic magnetic charged density $\rho_{NLED}$$(r)$ which is needed to calculate the magnetic mass of the slowly rotating Kerr-BH. We showed the mass profile $M(r)$ of the BH for different combinations of magnetic charges~($q_m$) and non-linear parameter ($\beta$) presence in the Lagrangian density. We found that $M(r)$ attains a plateau for values of $r$ close to the the cosmological length~($L$), where $L^2$= $\pm \frac{\Lambda}{3}$, irrespective of the combinations of $q_m$ and $\beta$. The $\pm$ sign corresponds to the de-Sitter(dS) and Anti-de-Sitter(AdS) respectively. Afterwards we showed the allowed parameter spaces in $a$-$M$ plane using sharkfin diagram for different values of $L$ with positive values of the horizon function, $\Delta(r)$, and explain the extremal criterion and asymptotic limit. We showed the values of $r$ where the horizon function of the quadratic polynomials becomes zero and called them as the inner(Cauchy), outer(Event) and large cosmological horizons with different values of $a$. We showed that the horizon structure depends on $a$, $L$ and the mass profile $M(r)$. Finally, we tabulated the numerical values of three thermodynamic parameter, i.e., $T$, $\Omega_h$ and $S$ at those horizons surfaces. Our results demonstrate that NLED with cosmological constant significantly modifies both the internal structure and thermodynamic properties of Kerr-BH.