Abstract
We study gravitational waves from a hierarchical three-body system up to first-order postNewtonian approximation. Under certain conditions, the existence of a nearby third body can cause periodic exchange between eccentricity of an inner binary and relative inclination, known as Kozai-Lidov oscillations. We analyze features of the waveform from the inner binary system undergoing such oscillations. We find that variation caused due to the tertiary companion can be observed in the gravitational waveforms and energy spectra, which should be compared with those from isolated binaries and coplanar three-body system. The detections from future space interferometers will make possible the investigation of the gravitational wave spectrum in mHz range and may fetch signals by sources addressed.
Highlights
The LIGO-VIRGO collaboration observed eleven gravitational wave signals from compact binary mergers during the first and second runs (O1 and O2) [1]
We find that variation caused due to the tertiary companion can be observed in the gravitational waveforms and energy spectra, which should be compared with those from isolated binaries and coplanar three-body system
Several big projects have been proposed in space; Big Bang Observer (BBO) [9], advanced Laser Interferometer Space Antenna (LISA) [10], and
Summary
The LIGO-VIRGO collaboration observed eleven gravitational wave signals from compact binary mergers during the first and second runs (O1 and O2) [1]. The GW signal would be distinguished by a net phase change or even a time-dependent Doppler shift arising from the orbital motion This could provide direct information about the black hole binary environments and otherwise invisible ambient mass. Recent work analyzes triple systems composed of the SMBH near the galactic center and a pair of BHs with different masses, from stellar to intermediate-mass BHs (IMBHs) [28,52]. They identify frequency peaks and examine the detectability of GWs with LISA, μAres, and DECIGO by integrating over the observation time within the lifetime of different GW detectors. We present the characteristic strains for all other models in Appendix B
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Free) 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
