New public code for initial data of unequal-mass, spinning compact-object binaries
Abstract
The construction of constraint-satisfying initial data is an essential element for the numerical exploration of the dynamics of compact-object binaries. While several codes have been developed over the years to compute generic quasiequilibrium configurations of binaries comprising either two black holes, or two neutron stars, or a black hole and a neutron star, these codes are often not publicly available or they provide only a limited capability in terms of mass ratios and spins of the components in the binary. We here present a new open-source collection of spectral elliptic solvers that are capable of exploring the major parameter space of binary black holes (BBHs), binary neutron stars (BNSs), and mixed binaries of black holes and neutron stars (BHNSs). Particularly important is the ability of the spectral-solver library to handle neutron stars that are either irrotational or with an intrinsic spin angular momentum that is parallel to the orbital one. By supporting both analytic and tabulated equations of state at zero or finite temperature, the new infrastructure is particularly geared toward allowing for the construction of BHNS and BNS binaries. For the latter, we show that the new solvers are able to reach the most extreme corners in the physically plausible space of parameters, including extreme mass ratios and spin asymmetries, thus representing the most extreme BNS computed to date. Through a systematic series of examples, we demonstrate that the solvers are able to construct quasiequilibrium and eccentricity-reduced initial data for BBHs, BNSs, and BHNSs, achieving spectral convergence in all cases. Furthermore, using such initial data, we have carried out evolutions of these systems from the inspiral to after the merger, obtaining evolutions with eccentricities ≲ 10⁻⁴−10⁻³, and accurate gravitational waveforms.
Additional Information
© 2021 American Physical Society. E. R. M. gratefully acknowledges support from a joint fellowship at the Princeton Center for Theoretical Science, the Princeton Gravity Initiative and the Institute for Advanced Study. The authors gratefully acknowledge the Gauss Centre for Supercomputing e.V.[155] for funding this project by providing computing time on the GCS Supercomputer SuperMUC at Leibniz Supercomputing Centre [156]. Part of the simulations were performed on the national supercomputer HPE Apollo Hawk at the High Performance Computing Center Stuttgart (HLRS) under the Grant No. BBHDISKS. L. R. gratefully acknowledges support from HGS-HIRe for FAIR and "PHAROS", COST Action No. CA16214.Attached Files
Published - PhysRevD.104.024057.pdf
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Additional details
- Eprint ID
- 121221
- Resolver ID
- CaltechAUTHORS:20230501-297257000.40
- Princeton University
- Institute for Advanced Study
- Helmholtz Graduate School for Hadron and Ion Research
- CA16214
- European Cooperation in Science and Technology (COST)
- Created
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2023-05-02Created from EPrint's datestamp field
- Updated
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2023-05-02Created from EPrint's last_modified field