Speaker
Description
We construct the canonical ensemble of a Reissner-Nordström black hole in a cavity for an arbitrary number of dimensions. The system of a charged black hole in a cavity can be described by a partition function given by the Euclidean path integral approach, where we consider the usual Einstein-Maxwell action with the Gibbons-Hawking-York boundary term and an additional boundary term of the Maxwell tensor. The spacetime is then Euclideanized and time becomes periodic. The inverse temperature at the boundary is fixed, which corresponds to the total time length at the cavity, and the charge is also fixed, which corresponds to the flux of the Maxwell tensor at the cavity. The zero loop aproximation is performed, and the path integral is heavily simplified, which allows us to find the black hole solutions for the fixed quantities. We find that, below a critical electric charge, there are three solutions, from which two are stable. Above the critical charge, there is only one solution, which is stable. We find analytical expressions for the points where these solutions meet and for the critical charge. Regarding thermodynamics, the energy, the pressure, the entropy and the electric potential are obtained. Stable solutions correspond to the solutions with positive heat capacity at constant charge. We analyze the favorable states and compare the gravitational radius of the zero action solutions between the canonical ensemble, the grand canonical ensemble and the Buchdahl-Andréasson-Wright bound. We verify that these three gravitational radii only coincide in the chargeless case and in the extreme case.
