Initial Conditions for Numerical Relativity -- Introduction to numerical methods for solving elliptic PDEs

Abstract

Numerical relativity became a powerful tool to investigate the dynamics of binary problems with black holes or neutron stars as well as the very structure of General Relativity. Although public numerical relativity codes are available to evolve such systems, a proper understanding of the methods involved is quite important. Here we focus on the numerical solution of elliptic partial differential equations. Such equations arise when preparing initial data for numerical relativity, but also for monitoring the evolution of black holes. Because such elliptic equations play an important role in many branches of physics, we give an overview of the topic, and show how to numerically solve them with simple examples and sample codes written in C++ and Fortran90 for beginners in numerical relativity or other fields requiring numerical expertise.

Lecture notes from the NRHEP spring school held at IST-Lisbon, March 2013. Extra material and notebooks available online at http://blackholes.ist.utl.pt/nrhep2/ To be published by IJMPA (V. Cardoso, L. Gualtieri, C. Herdeiro and U. Sperhake, Eds., 2013)

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Cited by in corpus (9)

• Advanced Methods in Black-Hole Perturbation Theory
• Numerical Methods for Finding Stationary Gravitational Solutions
• Black holes and fundamental fields in Numerical Relativity: initial data construction and evolution of bound states
• An Introduction to Well-posedness and Free-evolution
• Collapse of self-interacting fields in asymptotically flat spacetimes: do self-interactions render Minkowski spacetime unstable?
• A numerical relativity scheme for cosmological simulations
• Lecture Notes: Numerical Relativity in higher dimensional spacetimes
• Black holes and fundamental fields: hair, kicks and a gravitational "Magnus" effect
• Simple Numerical Solutions to the Einstein Constraints on Various Three-Manifolds