Binary neutron stars with generic spin, eccentricity, mass ratio, and compactness: Quasi-equilibrium sequences and first evolutions
Information about the last stages of a binary neutron star inspiral and the final merger can be extracted from quasiequilibrium configurations and dynamical evolutions. In this article, we construct quasiequilibrium configurations for different spins, eccentricities, mass ratios, compactnesses, and equations of state. For this purpose we employ the sgrid code, which allows us to construct such data in previously inaccessible regions of the parameter space. In particular, we consider spinning neutron stars in isolation and in binary systems; we incorporate new methods to produce highly eccentric and eccentricity-reduced data; we present the possibility of computing data for significantly unequal-mass binaries with mass ratios q≃2; and we create equal-mass binaries with individual compactness up to
© 2015 American Physical Society. (Received 29 July 2015; published 1 December 2015) It is a pleasure to thank Roland Haas, Michael Kramer, Alessandro Nagar, Jan Steinhoff, Thomas Tauris, and Maximiliano Ujevic for helpful discussions and valuable comments. We are particularly indebted to Patricia Schmidt for her help understanding the precession effects on the waveform. This work was supported in part by DFG grant SFB/Transregio 7 "Gravitational Wave Astronomy," the Graduierten-Akademie Jena, and the DFG Research Training Group 1523/1 "Quantum and Gravitational Fields." N. K. J.-M. acknowledges support from the AIRBUS Group Corporate Foundation through a chair in "Mathematics of Complex Systems" at the International Centre for Theoretical Sciences. S. B. acknowledges partial support from the National Science Foundation under grant numbers NSF AST-1333520, PHY-1404569, and AST-1205732. C. M. was supported by the STFC grant PP / E001025 / 1. W. T. was supported by the National Science Foundation under grant PHY-1305387. The authors also gratefully acknowledge the Gauss Centre for Supercomputing e.V. for funding this project by providing computing time on the GCS Supercomputer SuperMUC at Leibniz Supercomputing Centre and the computing time granted by the John von Neumann Institute for Computing provided on the supercomputer JUROPA at Jülich Supercomputing Centre. We also acknowledge usage of computer time on the Fermi CINECA machine allocated through the ISCRA initiative. Additionally, this work used the Extreme Science and Engineering Discovery Environment, which is supported by National Science Foundation grant number ACI-1053575, computer resources at the Institute of Theoretical Physics of the University of Jena, and the HPC cluster KOKO at Florida Atlantic University.
Published - PhysRevD.92.124007.pdf