2013/11/30 by D. Simakov, D. A. Simakov · 9 citations
Physics and Astronomy · #Acoustics #Advanced Frequency and Time Standards #Amplitude #Astrophysics #Chirp #Computer science #Detector #Frequency domain #Gravitational wave #Interferometry #Laser #Noise (video) #Optics #Physics #Pulsars and Gravitational Waves Research #SIGNAL (programming language) #Stellar, planetary, and galactic studies #gr-qc
paper · pdf · doi:10.1103/physrevd.90.102003
published in Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields 90(10) (American Physical Society) · Deeply revised according to the feed backs of two referees from PRD. The better structure was introduced. Number of consistency checks were added. 24 pages, 15 figures
openalex publication_date 2014/11/14 · arxiv created 2015/04/28 · arxiv updated 2015/04/29 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
In this article, we study a particular method of detection of chirp signals from coalescing compact binary stars---the so-called dynamical tuning, i.e., amplification of the signal via tracking of its instantaneous frequency by the tuning of a signal-recycled detector. The motion of the signal-recycling mirror, the position of which defines the tuning of the detector, causes nonstationarity of the detector. The dynamically tuned detector can be simulated in a quasistationary approximation if the mirror position, amplitude, and frequency of a chirp signal are changing slowly. A time-domain consideration developed for signal-recycled interferometers, in particular GEO 600, describes the signal and noise evolution in the more general case of a purely nonstationary detector. We prove that the shot noise from the dark port and optical losses remains white in this case. The analysis of the transient effects shows that during the perfect tracking of the chirp frequency only transients from fast amplitude changes arise because the transients from changes of the detector tuning and signal frequency completely cancel each other. The slow change of the amplitude in this case establishes a so-called virtually stationary detection, meaning the signal fields at the detector hold their stationary values at each instance of time, corresponding to the instantaneous parameters of the gravitational wave and of the detector. The signal-to-noise-ratio gain from the implementation of dynamical tuning, calculated in this paper, is \ensuremath∼17 for a shot noise-limited GEO 600-like detector and \ensuremath∼7 for a detector with both shot and displacement noise.