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Thermodynamic geometry of charged rotating black holes in Einsteinian cubic gravity

Aghil Keshavarzi

https://orcid.org/0009-0003-2711-3128

Department of Physics, University of Mohaghegh Ardabili, P.O. Box 179, Ardabil, Iran

E-mail Address: a.keshavarzi@uma.ac.ir

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Zahra Ebadi

https://orcid.org/0000-0002-5131-8700

Department of Physics, University of Mohaghegh Ardabili, P.O. Box 179, Ardabil, Iran

E-mail Address: z.ebadi@uma.ac.ir

Corresponding author.

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, and

Hosein Mohammadzadeh

https://orcid.org/0000-0003-0963-407X

Department of Physics, University of Mohaghegh Ardabili, P.O. Box 179, Ardabil, Iran

E-mail Address: mohammadzadeh@uma.ac.ir

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https://doi.org/10.1142/S0219887824502748Cited by:0 (Source: Crossref)

Abstract

We study the thermodynamic geometry of two types of asymptotically anti-de Sitter black holes in four-dimensional Einsteinian cubic gravity, including the uncharged rotating and charged non-rotating black holes, applying the Ruppeiner thermodynamic geometry method. The divergence of the scalar curvature of the Ruppeiner metric ( $R^{R}$ $R^{R}$ ) is found to be related to the vanishing of the heat capacity. The stability of the solutions is shown to be affected by the Einsteinian cubic gravity coupling constant $λ$ $λ$ . In the unstable phase of the rotating black hole, the $R^{R}$ $R^{R}$ appeared to possess additional diverging points, where the number of these points and the behavior of $R^{R}$ $R^{R}$ are controlled by the angular momentum parameter. Also, for the charged non-rotating black hole case, we show that depending on the values of $λ$ $λ$ , the solution may enjoy two types of phase transition and $R^{R}$ $R^{R}$ behaviors. The characteristic behavior of $R^{R}$ $R^{R}$ of these two types of black holes enabled us to recognize the types of interactions between microscopic degrees of freedom.

Keywords:

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