Numerical Relativity: Solving Einstein's Equations on the Computer

By E. Gourgoulhon. 2011

405 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/705ad9e09a3245b81ec5aea64757f25b0146411b

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In Astronomy and Astrophysics

1. Kent Yagi
2. N. Yunes
3. Emanuele Berti
4. Christian D. Ott
5. Pablo Laguna
6. Ian Hinder
7. Heling Deng
8. R. Cai

Citations in the corpus

• Primordial black hole formation by vacuum bubbles (2017, neutral): “In our coordinate system [25], Θout ∝ U + Γ R , Θin ∝ U − Γ R .”
• The Einstein Toolkit: a community computational infrastructure for relativistic astrophysics (2011, methodology): “For this, the Baumgarte-Shapiro-ShibataNakamura (BSSN) conformal-tracefree reformulation [9, 10, 149] of the original ArnowittDeser-Misner (ADM) formalism [129] is employed.”
• The 1965 Penrose singularity theorem (2014, positive): “Indeed, the presence of OTS on spatial slices is the signal used in numerical relativity to detect black holes [14].”
• Primordial black hole and wormhole formation by domain walls (2016, methodology): “A well known drawback of the geodesic slicing that we are using is that it inevitably hits the singularity [15].”
• Comprehensive nucleosynthesis analysis for ejecta of compact binary mergers (2014, neutral): “…to the construction of BH–BH or NS–BH binary initial data necessary for fully relativistic calculations (see e.g. Kyutoku, Shibata & Taniguchi 2009; Baumgarte & Shapiro 2010; Bauswein 2010, where the corresponding formulae can be found; see also Faber et al. 2006 for a similar approach within…”
• The Gravitational-Wave Physics (2017, background): “1 Post-Newtonian Approximation Based on quadrupole formula [144], we can estimate the GWs related to a binary system: h+ = − M r 2Ω(2)R(2)(1 + cos(2) θ) cos[2Ω(t− r)], (4.”
• Extreme gravity tests with gravitational waves from compact binary coalescences: (I) inspiral–merger (2018, background): “A stable evolution of binary black holes and neutron stars in numerical relativity requires an understanding of many complex issues, such as the well-posedness of the evolution system, the construction of initial data and gauge conditions [285].”