MHD of rotating compact stars with spectral methods: description of the algorithm and tests

TL;DR

This paper introduces a spectral code for simulating general relativistic magnetohydrodynamics in rotating compact stars, emphasizing the algorithmic approach and potential astrophysical applications.

Contribution

The paper presents a new spectral code tailored for relativistic MHD in rotating compact stars, utilizing the relativistic anelastic approximation and highlighting algorithmic innovations.

Findings

Demonstrates the code's effectiveness through illustrative tests

Shows potential for astrophysical applications in star physics

Highlights advantages of spectral methods in this context

Abstract

A flexible spectral code for the study of general relativistic magnetohydrodynamics is presented. Aiming at investigating the physics of slowly rotating magnetized compact stars, this new code makes use of various physically motivated approximations. Among them, the relativistic anelastic approximation is a key ingredient of the current version of the code. In this article, we mainly outline the method, putting emphasis on algorithmic techniques that enable to benefit as much as possible of the non-dissipative character of spectral methods, showing also a potential astrophysical application and providing a few illustrative tests.