BSSN equations in spherical coordinates without regularization: vacuum and non-vacuum spherically symmetric spacetimes

TL;DR

This paper presents a numerical implementation of the BSSN equations in spherical coordinates without regularization, successfully evolving vacuum and non-vacuum spherically symmetric spacetimes, including black hole formation, using a partially implicit Runge-Kutta method.

Contribution

The authors develop a stable, regularization-free numerical code for BSSN equations in spherical symmetry employing a partially implicit Runge-Kutta scheme, enabling accurate simulations of relativistic phenomena.

Findings

Stable evolutions of regular spacetimes without regularization.

Successful simulation of black hole formation from stellar collapse.

Demonstrated convergence and accuracy through various tests.

Abstract

Brown has recently introduced a covariant formulation of the BSSN equations which is well suited for curvilinear coordinate systems. This is particularly desirable as many astrophysical phenomena are symmetric with respect to the rotation axis or are such that curvilinear coordinates adapt better to their geometry. However, the singularities associated with such coordinate systems are known to lead to numerical instabilities unless special care is taken (e.g., regularization at the origin). Cordero-Carrion will present a rigorous derivation of partially implicit Runge-Kutta methods in forthcoming papers, with the aim of treating numerically the stiff source terms in wave-like equations that may appear as a result of the choice of the coordinate system. We have developed a numerical code solving the BSSN equations in spherical symmetry and the general relativistic hydrodynamic equations written in flux-conservative form. A key feature of the code is that it uses a second-order partially implicit Runge-Kutta method to integrate the evolution equations. We perform and discuss a number of tests to assess the accuracy and expected convergence of the code, namely a pure gauge wave, the evolution of a single black hole, the evolution of a spherical relativistic star in equilibrium, and the gravitational collapse of a spherical relativistic star leading to the formation of a black hole. We obtain stable evolutions of regular spacetimes without the need for any regularization algorithm at the origin.