The initial value problem as it relates to numerical relativity

TL;DR

This paper discusses the initial value problem in numerical relativity, focusing on how to specify and construct initial data for spacetime simulations involving black holes and neutron stars, using conformal decompositions and quasi-equilibrium assumptions.

Contribution

It reviews methods for constructing initial data satisfying Einstein's constraints, especially for binary systems, using conformal decompositions and quasi-equilibrium approximations.

Findings

Conformal decompositions facilitate the construction of constraint-satisfying initial data.

Quasi-equilibrium assumptions simplify the elliptic equations for binary systems.

Initial data for black holes and neutron stars can be effectively generated for numerical simulations.

Abstract

Spacetime is foliated by spatial hypersurfaces in the 3+1 split of General Relativity. The initial value problem then consists of specifying initial data for all relevant fields on one such a spatial hypersurface. These fields are the 3-metric and extrinsic curvature together with matter fields such as fluid velocity, energy density and rest mass density. There is a lot of freedom in choosing such initial data. This freedom corresponds to the physical state of the system at the initial time. At the same time the initial data have to satisfy the Hamiltonian and momentum constraint equations of General Relativity and can thus not be chosen completely freely. We discuss the conformal transverse traceless and conformal thin sandwich decompositions that are commonly used in the construction of constraint satisfying initial data. These decompositions allow us to specify certain free data that describe the physical nature of the system. The remaining metric fields are then determined by solving elliptic equations derived from the constraint equations. We describe initial data for single black holes and single neutron stars, and how we can use conformal decompositions to construct initial data for binaries made up of black holes or neutron stars. Orbiting binaries will emit gravitational radiation and thus lose energy. Since the emitted radiation tends to circularize the orbits over time, one can thus expect that the objects in a typical binary move on almost circular orbits with slowly shrinking radii. This leads us to the concept of quasi-equilibrium which essentially assumes that time derivatives are negligible in corotating coordinates, for binaries on almost circular orbits. We review how quasi-equilibrium assumptions can be used to make physically well motivated approximations that simplify the elliptic equations we have to solve.