Implementing an apparent-horizon finder in three dimensions

TL;DR

This paper generalizes a promising apparent-horizon finding scheme for 3D numerical spacetimes, enabling adjustable accuracy through higher-order tensor expansions and providing recurrence relations for efficient computation.

Contribution

It extends the symmetric trace-free tensor expansion method for apparent-horizon finding to arbitrary order with new recurrence relations, improving accuracy control.

Findings

Successfully calibrated the generalized scheme in black-hole spacetimes

Demonstrated the method's ability to achieve desired accuracy levels

Provided a practical implementation for 3D numerical relativity simulations

Abstract

Locating apparent horizons is not only important for a complete understanding of numerically generated spacetimes, but it may also be a crucial component of the technique for evolving black-hole spacetimes accurately. A scheme proposed by Libson et al., based on expanding the location of the apparent horizon in terms of symmetric trace-free tensors, seems very promising for use with three-dimensional numerical data sets. In this paper, we generalize this scheme and perform a number of code tests to fully calibrate its behavior in black-hole spacetimes similar to those we expect to encounter in solving the binary black-hole coalescence problem. An important aspect of the generalization is that we can compute the symmetric trace-free tensor expansion to any order. This enables us to determine how far we must carry the expansion to achieve results of a desired accuracy. To accomplish this generalization, we describe a new and very convenient set of recurrence relations which apply to symmetric trace-free tensors.