A No-Boundary Method for Numerical Relativity
arXiv:1905.08657 · doi:10.1088/1361-6382/ab5e99
Abstract
We propose a method for numerical relativity in which the spatial grid is finite and no outer boundary condition is needed. As a "proof of concept" we implement this method for the case of a self-gravitating, spherically symmetric scalar field.
References in corpus (14)
- On the Numerical Integration of Einstein's Field Equations
- A catalog of 174 binary black-hole simulations for gravitational-wave astronomy
- Harmonic coordinate method for simulating generic singularities
- Simulation of Binary Black Hole Spacetimes with a Harmonic Evolution Scheme
- High-powered Gravitational News
- Understanding critical collapse of a scalar field
- Numerical Relativity in Spherical Polar Coordinates: Evolution Calculations with the BSSN Formulation
- Scaling of curvature in sub-critical gravitational collapse
- Problems which are well-posed in a generalized sense with applications to the Einstein equations
- Numerical evolution of Brill waves
- Regularity of the Einstein Equations at Future Null Infinity
- Numerical treatment of the hyperboloidal initial value problem for the vacuum Einstein equations. I. The conformal field equations
- Well-posed initial-boundary value problem for the harmonic Einstein equations using energy estimates
- Numerical evolution of plane gravitational waves in the Friedrich-Nagy gauge