Higher dimensional numerical relativity: Code comparison
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Higher dimensional numerical relativity : Code comparison. / Witek, Helvi; Okawa, Hirotada; Cardoso, Vitor; Gualtieri, Leonardo; Herdeiro, Carlos; Shibata, Masaru; Sperhake, Ulrich; Zilhao, Miguel.
In: Physical Review D, Vol. 90, No. 8, 084014, 10.10.2014.Research output: Contribution to journal › Journal article › Research › peer-review
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TY - JOUR
T1 - Higher dimensional numerical relativity
T2 - Code comparison
AU - Witek, Helvi
AU - Okawa, Hirotada
AU - Cardoso, Vitor
AU - Gualtieri, Leonardo
AU - Herdeiro, Carlos
AU - Shibata, Masaru
AU - Sperhake, Ulrich
AU - Zilhao, Miguel
PY - 2014/10/10
Y1 - 2014/10/10
N2 - The nonlinear behavior of higher dimensional black hole spacetimes is of interest in several contexts, ranging from an understanding of cosmic censorship to black hole production in high-energy collisions. However, nonlinear numerical evolutions of higher dimensional black hole spacetimes are tremendously complex, involving different diagnostic tools and "dimensional reduction methods." In this work we compare two different successful codes to evolve Einstein's equations in higher dimensions, and show that the results of such different procedures agree to numerical precision, when applied to the collision from rest of two equal-mass black holes. We calculate the total radiated energy to be E-rad/M = (9.0 +/- 0.5) x 10(-4) in five dimensions and E-rad/M = (8.1 +/- 0.4) x 10(-4) in six dimensions.
AB - The nonlinear behavior of higher dimensional black hole spacetimes is of interest in several contexts, ranging from an understanding of cosmic censorship to black hole production in high-energy collisions. However, nonlinear numerical evolutions of higher dimensional black hole spacetimes are tremendously complex, involving different diagnostic tools and "dimensional reduction methods." In this work we compare two different successful codes to evolve Einstein's equations in higher dimensions, and show that the results of such different procedures agree to numerical precision, when applied to the collision from rest of two equal-mass black holes. We calculate the total radiated energy to be E-rad/M = (9.0 +/- 0.5) x 10(-4) in five dimensions and E-rad/M = (8.1 +/- 0.4) x 10(-4) in six dimensions.
KW - BLACK-HOLES
KW - GRAVITATIONAL PERTURBATIONS
KW - CARTESIAN GRIDS
KW - STABILITY
KW - EQUATIONS
KW - ISOMETRY
KW - STRINGS
KW - SYSTEMS
KW - FIELD
U2 - 10.1103/PhysRevD.90.084014
DO - 10.1103/PhysRevD.90.084014
M3 - Journal article
VL - 90
JO - Physical Review D
JF - Physical Review D
SN - 2470-0010
IS - 8
M1 - 084014
ER -
ID: 300080045