Integrability of the Minimal Strain Equations for the Lapse and Shift in 3+1 Numerical Relativity

TL;DR

This paper establishes conditions under which the minimal strain equations for lapse and shift in 3+1 numerical relativity are well-posed, supporting their use for stable, slow-evolving coordinate systems in binary black hole simulations.

Contribution

It derives criteria for the strong ellipticity of the minimal strain equations, ensuring existence and uniqueness of solutions in numerical relativity contexts.

Findings

Criteria for strong ellipticity are satisfied in test-bed metrics.

Conditions are likely met in inspiraling binary scenarios.

The solutions are expected to be unique and reproducible numerically.

Abstract

Brady, Creighton and Thorne have argued that, in numerical relativity simulations of the inspiral of binary black holes, if one uses lapse and shift functions satisfying the ``minimal strain equations'' (MSE), then the coordinates might be kept co-rotating, the metric components would then evolve on the very slow inspiral timescale, and the computational demands would thus be far smaller than for more conventional slicing choices. In this paper, we derive simple, testable criteria for the MSE to be strongly elliptic, thereby guaranteeing the existence and uniqueness of the solution to the Dirichlet boundary value problem. We show that these criteria are satisfied in a test-bed metric for inspiraling binaries, and we argue that they should be satisfied quite generally for inspiraling binaries. If the local existence and uniqueness that we have proved holds globally, then, for appropriate boundary values, the solution of the MSE exhibited by Brady et. al. (which tracks the inspiral and keeps the metric evolving slowly) will be the unique solution and thus should be reproduced by (sufficiently accurate and stable) numerical integrations.