Geometrodynamics of Schwarzschild black holes
Geometrodynamics of Schwarzschild black holes
The curvature coordinates T, R of a Schwarzschild spacetime are turned into canonical coordinates T(r), ssR(r) on the phase space of spherically symmetric black holes. The entire dynamical content of the Hamiltonian theory is reduced to the constraints requiring that the momenta ${\mathit{P}}_{\mathit{T}}$(r), ${\mathit{P}}_{\mathit{s}\mathit{s}\mathit{R}}$(r) vanish. What remains is a conjugate …