High-accuracy simulations of highly spinning binary neutron star systems
- With an increasing number of expected gravitational-wave detections of binary neutron star mergers, it is essential that gravitational-wave models employed for the analysis of observational data are able to describe generic compact binary systems. This includes systems in which the individual neutron stars are millisecond pulsars for which spin effects become essential. In this work, we perform numerical-relativity simulations of binary neutron stars with aligned and antialigned spins within a range of dimensionless spins of chi similar to [-0.28, 0.58]. The simulations are performed with multiple resolutions, show a clear convergence order and, consequently, can be used to test existing waveform approximants. We find that for very high spins gravitational-wave models that have been employed for the interpretation of GW170817 and GW190425 arc not capable of describing our numerical-relativity dataset. We verify through a full parameter estimation study in which clear biases in the estimate of the tidal deformability and effective spinWith an increasing number of expected gravitational-wave detections of binary neutron star mergers, it is essential that gravitational-wave models employed for the analysis of observational data are able to describe generic compact binary systems. This includes systems in which the individual neutron stars are millisecond pulsars for which spin effects become essential. In this work, we perform numerical-relativity simulations of binary neutron stars with aligned and antialigned spins within a range of dimensionless spins of chi similar to [-0.28, 0.58]. The simulations are performed with multiple resolutions, show a clear convergence order and, consequently, can be used to test existing waveform approximants. We find that for very high spins gravitational-wave models that have been employed for the interpretation of GW170817 and GW190425 arc not capable of describing our numerical-relativity dataset. We verify through a full parameter estimation study in which clear biases in the estimate of the tidal deformability and effective spin are present. We hope that in preparation of the next gravitational-wave observing run of the Advanced LIGO and Advanced Virgo detectors our new set of numerical-relativity data can be used to support future developments of new gravitational-wave models.…
Author details: | Reetika DudiORCiDGND, Tim DietrichORCiDGND, Alireza RashtiORCiD, Bernd BrügmannORCiD, Jan SteinhoffORCiD, Wolfgang TichyORCiD |
---|---|
DOI: | https://doi.org/10.1103/PhysRevD.105.064050 |
ISSN: | 2470-0010 |
ISSN: | 2470-0029 |
Title of parent work (English): | Physical review : D, Particles, fields, gravitation, and cosmology |
Publisher: | American Physical Society |
Place of publishing: | College Park |
Publication type: | Article |
Language: | English |
Date of first publication: | 2022/03/28 |
Publication year: | 2022 |
Release date: | 2024/05/17 |
Volume: | 105 |
Issue: | 6 |
Article number: | 064050 |
Number of pages: | 13 |
Funding institution: | Max Planck Society; DFG [BR 2176/5-1]; National Science Foundation; [PHY-1707227, PHY-2011729]; High-Performance Computing Center Stuttgart; (HLRS) [GWanalysis 44189]; Leibniz Super-computing Centre (LRZ) [pn29ba] |
Organizational units: | Mathematisch-Naturwissenschaftliche Fakultät / Institut für Physik und Astronomie |
DDC classification: | 5 Naturwissenschaften und Mathematik / 53 Physik / 530 Physik |
Peer review: | Referiert |
Publishing method: | Open Access / Hybrid Open-Access |
License (German): | CC-BY - Namensnennung 4.0 International |