Source term method for binary neutron stars initial data

TL;DR

This paper introduces a new Cartesian grid-based method for solving the fluid Poisson equation in binary neutron star initial data, avoiding complex boundary-fitted coordinates and handling singularities effectively.

Contribution

A novel source term method for binary neutron star initial data that simplifies boundary handling and improves computational efficiency in numerical relativity.

Findings

Demonstrated convergence in 2D tests.

Achieved approximately 1% agreement with existing solvers.

Applicable to 3D realistic binary neutron star problems.

Abstract

The initial condition problem for a binary neutron star system requires a Poisson equation solver for the velocity potential with a Neumann-like boundary condition on the surface of the star. Difficulties that arise in this boundary value problem are: a) the boundary is not known a-priori, but constitutes part of the solution of the problem; b) various terms become singular at the boundary. In this work, we present a new method to solve the fluid Poisson equation for irrotational/spinning binary neutron stars. The advantage of the new method is that it does not require complex fluid surface fitted coordinates and it can be implemented in a Cartesian grid, which is a standard choice in numerical relativity calculations. This is accomplished by employing the source term method proposed by Towers, where the boundary condition is treated as a jump condition and is incorporated as additional source terms in the Poisson equation, which is then solved iteratively. The issue of singular terms caused by vanishing density on the surface is resolved with an additional separation that shifts the computation boundary to the interior of the star. We present two-dimensional tests to show the convergence of the source term method, and we further apply this solver to a realistic three-dimensional binary neutron star problem. By comparing our solution with the one coming from the initial data solver COCAL, we demonstrate agreement to approximately $1\%$. Our method can be used in other problems with non-smooth solutions like in magnetized neutron stars.