2001/02/07 by Mirta S. Iriondo, Oscar Reula, Oscar A. Reula
Mathematics · Physics and Astronomy · #Black Holes and Theoretical Physics #Classical mechanics #Cosmology and Gravitation Theories #Geometry #Mathematical analysis #Mathematics #Physics #Pulsars and Gravitational Waves Research #Scalar (mathematics) #Scalar field #Simple (philosophy) #gr-qc
paper · pdf · doi:10.1103/physrevd.65.044024
published as Phys.Rev. D65 (2002) 044024 · 15 pages, 15 figures
arxiv created 2001/02/07 · openalex publication_date 2002/01/28 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We perform a numerical free evolution of a self-gravitating, spherically symmetric scalar field satisfying the wave equation. The evolution equations can be written in a very simple form and are symmetric hyperbolic in the Eddington-Finkelstein coordinates. The simplicity of the system allows us to display and deal with the typical gauge instability present in these coordinates. The numerical evolution is performed with a standard method of lines, fourth order in space and time. The evolution is performed using the standard Runge-Kutta method while the space discrete derivative is symmetric (nondissipative). The constraints are preserved, within numerical errors, by the evolution and we are able to reproduce several known results.