Gravitational wave detector

Geodesy Gravitational Wave Detectors Gravitational Wave Physics Mechanics, Classical Remote Sensing erom Satellites... 

Detectors Gravitational Wave Physics Infrared Astronomy Neutrino Astronomy Pulsars Radio Astronomy, Interferometry Supernovae Ultraviolet Space Astronomy X-Ray Astronomy... 

Abstract This is an introduction to gravitational wave astronomy. The physical bases of gravitation and the generation and detection of gravitational waves are recalled and then kilometric detectors under construction are described. 

We now end the theoretical description of gravitational waves, and start the practical description of gravitational wave detectors. 

Interferometric gravitational wave detectors 3.1 Properties of real optical detectors... 

Proc. of the International summer school on Experimental physics of gravitational waves, (Barone, M. et al. Eds., World Scientihc, London 2000). Contains a valuable chapter on General relativity by P. Tourrenc (contains a precise description of the various coordinates systems and their use, OBLIGATORY), a chapter by S. Bonazzola and E. Gourgoulhon on compact sources, in particular neutron stars, and a chapter by Jean-Yves Vinet on numerical simulations of interferometric gw detectors. 

Saulson, P.R.,1994, Fundamentals of interferometric gravitational wave detectors, (World Scientific, London), provides a very complete technical description of interferometric gravitational wave detectors. No previous knowledge in relativity is required. 

Fig. 16.1. Capacitive transducer for resonant gravitational waves detectors.

If a supernova emits gravitational waves as well as neutrinos, the gravitational waves will reach Earth-bound detectors slightly earlier because of the finite neutrino rest-mass. Assuming a supernova goes off at a distance of 100 Mpc, and a neutrino rest-mass of 0.1 eV, find the time delay for neutrino energies of 1 MeV and 10 MeV respectively. 

P. R. Saulson, Fundamentals of Interferometric Gravitational Wave Detectors, World Scientific, Singapore, 1994. 

The sensitivity of a gravitational wave detectors depends essentially on the stability and output power of the laser. In an improved version of the advanced LIGO detector called aLIGO the following laser system is used [1357]. 

Fig. 9.102 Gravitational wave detector based on a Michelson interferometer ...

Since their installation the aLIGO PSLs operate stable and provide reliable light sources for the gravitational wave detectors. 

In order to get an impression about the required characteristic data of a gravitational wave detector, in Table 9.1 the technical data of GEO 600 are compiled. 

T.M. Niebaum, A. Rudiger, R. SchiUing, L. Schnupp, W. Winkler, K. Danzmann, Pulsar search using data compression with the Garching gravitational wave detector. Phys. Rev. D 47,3106(1993)... 

The basic part of such a detector (Fig. 14.68) is a Michelson interferometer with long arms (several kilometers) and an extremely well stabilized laser. If a gravitational wave causes a length difference AL between the two arms of the interferometer, a phase difference A0 = (47t/A,) AL appears between the two partial waves at the exit of the interferometer. The minimum detectable phase change A0 is limited by the phase noise If laser delivers N photons hv per second, the two detectors measure the intensities... 

A. Wicht, K. Danzmann, M. Fleischhauer, M. Scully, G. Muller, R.-H. Rinkleff White-light cavities, atomic phase coherence and gravitational wave detectors. Opt. Commun. 134, 431 (1997)... 

Wicht A, Danzmann K, Fleischhauer M and et al. White-light cavities, atomic phase coherence, and gravitational wave detectors. Optics Communications 1997 Jan 15 134 431-439. 

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