Near-horizon symmetries of local black holes in general relativity

We analyze the near-horizon symmetries of static, axisymmetric, four-dimensional black holes with spherical and toroidal horizon topologies in vacuum general relativity. These black hole solutions, collectively referred to as local/distorted black holes, are known in closed form and are not asymptotically flat. Building on earlier works in the literature that primarily focused on black holes with spherical topology, we compute the algebra of the Killing vector fields that preserve the asymptotic structure near the horizons and the algebra of the associated Noether-Wald charges under the boundary conditions that produce the spin-$s$ ${\mathrm{BMS}}_{d}$ and the Heisenberg-like algebras. We show that a similar analysis extends to all local axisymmetric black holes. The toroidal topology of the holes changes the algebras considerably. For example, one obtains two copies of spin-$s$ ${\mathrm{BMS}}_{3}$ instead of spin-$s$ ${\mathrm{BMS}}_{4}$. We also revisit the thermodynamics of black holes under these boundary conditions. While previous studies suggested that spin-$s$ ${\mathrm{BMS}}_{d}$ preserves the first law of thermodynamics for isolated horizons ($\ensuremath{\kappa}=\text{const}$), our analysis indicates that this is not generally the case when the spin parameter $s$ is nonzero. A nonzero $s$ can be seen as introducing a conical singularity (in the Euclidean quantum gravity sense) or a Hamiltonian that causes soft hairs to contribute to the energy. This leads us to interpret the spin-$s$ ${\mathrm{BMS}}_{d}$ boundary condition as arising in the context of dynamical black holes.