学术文献库

We present a canonical Hamiltonian formulation of GR in which $τ$, the parameter of system evolution, is external to spacetime, playing a role similar to what we call time in nonrelativistic mechanics. This approach, known as Stueckelberg-Horwitz-Piron (SHP) theory, inherits the full computational power of classical analytical mechanics while maintaining manifest covariance throughout and eliminating possible conflict with general diffeomorphism invariance. In particular, SHP simplifies the initial value problem with potential applications in highly dynamical interactions, such as black hole collisions. By allowing the energy-momentum tensor and metric to depend explicitly on $τ$, we may describe particle motion in geodesic form with respect to a dynamically evolving background metric. As a toy model, we consider a $τ$-dependent mass $M(τ)$, first as a perturbation in the Newtonian approximation and then for a Schwarzschild-like metric. As expected, the extended Einstein equations imply a non-zero energy-momentum tensor, proportional to $dM / dτ$, representing a flow of mass and energy into spacetime that corresponds to the changing source mass. In $τ$-equilibrium, this system becomes a generalized Schwarzschild solution for which the extended Ricci tensor and energy-momentum tensor vanish.