2013/12/31 by Koutarou Kyutoku, N. Seto, Naoki Seto · 1 citation
Earth and Planetary Sciences · Physics and Astronomy · #Acoustics #Astrophysics #Binary number #Detector #Gamma-ray bursts and supernovae #Gravitational wave #Gravitational-wave observatory #Harmonic #High-pressure geophysics and materials #Neutron star #Noise (video) #Optics #Physics #Pulsars and Gravitational Waves Research #SIGNAL (programming language) #astro-ph.HE #gr-qc
paper · pdf · doi:10.1093/mnras/stu698
published as Mon. Not. R. Astron. Soc. 441, 1934-1942 (2014) · 10 pages, 5 figures, matched to the published version with additional references
openalex publication_date 2014/05/15 · arxiv created 2014/05/20 · openalex created_date 2016/06/24 · arxiv updated 2017/12/27 · openalex updated_date 2026/08/05
We study the possibility of pre-merger localization of eccentric compact binary coalescences by second-generation gravitational-wave detector networks. Gravitational waves from eccentric binaries can be regarded as a sequence of pulses, which are composed of various higher harmonic modes than ones with twice the orbital frequency. The higher harmonic modes from a very early inspiral phase will not only contribute to the signal-to-noise ratio, but also allow us to localize the gravitational-wave source before the merger sets in. This is due to the fact that high-frequency gravitational waves are essential for the source localization via triangulation by ground-based detector networks. We found that the single-detector signal-to-noise ratio exceeds 5 at 10 min before the merger for a 1.4–1.4 M⊙ eccentric binary neutron stars at 100 Mpc in optimal cases, and it can be localized up to 10 deg2 at half a minute before the merger by a four-detector network. We will even be able to achieve ∼10 deg2 at 10 min before the merger for a face-on eccentric compact binary by a five-detector network.