1 Introduction

Einstein’s equations represent a complicated set of nonlinear partial differential equations for which some exact [30] or approximate [31Jump To The Next Citation Point] analytical solutions are known. But these solutions are not always suitable for physically or astrophysically interesting systems, which require an accurate description of their relativistic gravitational field without any assumption on the symmetry or with the presence of matter fields, for instance. Therefore, many efforts have been undertaken to solve Einstein’s equations with the help of computers in order to model relativistic astrophysical objects. Within this field of numerical relativity, several numerical methods have been experimented with and a large variety are currently being used. Among them, spectral methods are now increasingly popular and the goal of this review is to give an overview (at the moment it is written or updated) of the methods themselves, the groups using them and the results obtained. Although some of the theoretical framework of spectral methods is given in Sections 2 to 4, more details can be found in the books by Gottlieb and Orszag [94Jump To The Next Citation Point], Canuto et al. [56Jump To The Next Citation Point, 57Jump To The Next Citation Point, 58Jump To The Next Citation Point], Fornberg [79Jump To The Next Citation Point], Boyd [48Jump To The Next Citation Point] and Hesthaven et al. [117Jump To The Next Citation Point]. While these references have, of course, been used for writing this review, they may also help the interested reader to get a deeper understanding of the subject. This review is organized as follows: hereafter in the introduction, we briefly introduce spectral methods, their usage in computational physics and give a simple example. Section 2 gives important notions concerning polynomial interpolation and the solution of ordinary differential equations (ODE) with spectral methods. Multidomain approach is also introduced there, whereas some multidimensional techniques are described in Section 3. The cases of time-dependent partial differential equations (PDE) are treated in Section 4. The last two sections then review results obtained using spectral methods: for stationary configurations and initial data (Section 5), and for the time evolution (Section 6) of stars, gravitational waves and black holes.

 1.1 About spectral methods
 1.2 Spectral methods in physics
 1.3 A simple example

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