MHD of rotating compact stars with spectral methods: description of the algorithm and tests
arXiv:gr-qc/0612049 · doi:10.1088/0264-9381/24/12/S15
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.
15 pages, 4 figures (new figure added, misprints corrected) Article accepted for publication in a special issue of Classical and Quantum Gravity "New Frontiers in Numerical Relativity"
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- A study on relativistic lagrangian field theories with non-topological soliton solutions
- General solution for the vacuum electromagnetic field in the surroundings of a rotating star
- A spectral method for the wave equation of divergence-free vectors and symmetric tensors inside a sphere
- Numerical relativity simulations in the era of the Einstein Telescope
- Luminosity of a quark star undergoing torsional oscillations and the problem of gamma ray bursts