Abstract
In this work, we study the thermodynamic geodesics of 4D asymptotically anti-de Sitter black holes in the context of the geometrothermodynamics (GTD) type II metric. We construct GTD type II metrics for four different black holes: 4D Kerr–Newman AdS (KN-AdS), Kerr-AdS (K-AdS), Reissner–Nordstrom AdS (RN-AdS), and Dyonic AdS black holes in various ensembles. For K-AdS and RN-AdS black holes, we work in canonical as well as grand canonical ensembles. For KN-AdS and Dyonic AdS black holes, in addition to these two ensembles, we also consider a fixed charged ensemble. For each case, we solve the corresponding geodesic equations numerically and analyze their behavior near the spinodal curves. These spinodal curves, which separate the positive specific heat region from the negative specific heat region, can be treated as the boundary between two black hole phases in the thermodynamic parameter space. The points on the spinodal curve are the points in parameter space at which we reach Davies’ temperature. We find that the geodesics, in all the cases under consideration, are confined to a single phase and exhibit either turning behavior or incompleteness near the spinodal curve (Davies’ temperature). This is universally true for GTD type II geodesics in KN-AdS, K-AdS, RN-AdS, and Dyonic AdS black holes in different ensembles. From this, we conclude that the turning behavior or incompleteness of geodesics in GTD type II geometry can be used as an indicator of phase transitions in 4D asymptotically AdS black holes.
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Appendix: Geodesic equations
Appendix: Geodesic equations
1.1 Kerr–Newman black hole
Geodesic equations for canonical ensemble:
and
where \(\dot{s}=\frac{\partial s}{\partial \tau }\), \(\ddot{s}=\frac{\partial ^2 s}{\partial \tau ^2}\), \(\dot{j}=\frac{\partial j}{\partial \tau }\), and \(\ddot{j}=\frac{\partial ^2 j}{\partial \tau ^2}\) with \(\tau\) being the affine parameter. Similar notation is used for the rest of the appendix.
Geodesic equations for grand canonical ensemble (in s vs \(\omega\) space):
and
Geodesic equations for grand canonical ensemble (in s vs \(\phi\) space):
and
Geodesic equations for fixed charged ensemble (in s vs \(\omega\) space):
and
where
and
Geodesic equations for fixed charged ensemble (in s vs q space):
and
where
and
1.2 2. Kerr-AdS black hole
Geodesic equations for canonical ensemble:
and
Geodesic equations for grand canonical ensemble:
and
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Gogoi, N.J., Mahanta, G.K. & Phukon, P. Geodesics in geometrothermodynamics (GTD) type II geometry of 4D asymptotically anti-de-Sitter black holes. Eur. Phys. J. Plus 138, 345 (2023). https://doi.org/10.1140/epjp/s13360-023-03938-x
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DOI: https://doi.org/10.1140/epjp/s13360-023-03938-x