ausblenden:
Schlagwörter:
General Relativity and Quantum Cosmology, gr-qc
Zusammenfassung:
Numerical relativity simulations of merging black holes provide the most
accurate description of the binary dynamics and the emitted gravitational wave
signal. However, practical considerations such as imperfect initial data and
initial parameters mean that achieving target parameters, such as the orbital
eccentricity or the black hole spin directions, at the beginning of the usable
part of the simulation is challenging. In this paper, we devise a method to
produce simulations with specific target parameters, namely the Keplerian
orbital parameters-eccentricity, semimajor axis, mean anomaly-and the black
hole spin vectors using SpEC. The method is an extension of the current process
for achieving vanishing eccentricity and it is based on a parameter control
loop that iteratively numerically evolves the system, fits the orbit with
analytical post-Newtonian equations, and calculates updated input parameters.
Through SpEC numerical simulations, we demonstrate $\lesssim 10^{-3}$ and
$O(\rm degree)$ convergence for the orbital eccentricity and the spin
directions respectively in $\leq7$ iterations. These tests extend to binaries
with mass ratios $q \leq 3$, eccentricities $e \leq 0.65$, and spin magnitudes
$|\chi | \leq 0.75$. Our method for controlling the orbital and spin parameters
of numerical simulations can be used to produce targeted simulations in
sparsely covered regions of the parameter space or study the dynamics of
relativistic binaries.
