2014年7月
Pre-merger localization of eccentric compact binary coalescences with second-generation gravitational-wave detector networks
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
- ,
- 巻
- 441
- 号
- 3
- 開始ページ
- 1934
- 終了ページ
- 1942
- 記述言語
- 英語
- 掲載種別
- 研究論文(学術雑誌)
- DOI
- 10.1093/mnras/stu698
- 出版者・発行元
- OXFORD UNIV PRESS
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-aS (TM) eccentric binary neutron stars at 100 Mpc in optimal cases, and it can be localized up to 10 deg(2) at half a minute before the merger by a four-detector network. We will even be able to achieve similar to 10 deg(2) at 10 min before the merger for a face-on eccentric compact binary by a five-detector network.
- リンク情報
- ID情報
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- DOI : 10.1093/mnras/stu698
- ISSN : 0035-8711
- eISSN : 1365-2966
- Web of Science ID : WOS:000338763600008