Computer Science – Sound
Scientific paper
Jan 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994phdt.........6z&link_type=abstract
Thesis (PH.D.)--STANFORD UNIVERSITY, 1994.Source: Dissertation Abstracts International, Volume: 55-10, Section: B, page: 4417.
Computer Science
Sound
3
Gravitational Waves, Antenna
Scientific paper
The sensitivity of resonant-mass gravitational radiation detectors depends on both the antenna cross-section and the detector noise. The cross-section is determined by the sound velocity VS and density rho of the antenna material, as well as the antenna geometry. The principal detector noise sources are thermal Nyquist noise and noise due to the readout electromechanical amplifier. The cross-section is proportional to rho V_sp{S}{5} for a given frequency and antenna geometry while the thermal noise is inversely proportional to the antenna's mechanical quality factor Q for a given temperature. Materials with high VS could, in principle, provide about a hundred-fold increase in the antenna cross -section as compared to current generation detectors. In this dissertation we report the results of measurements of the temperature-dependent mechanical losses in several suitable high sound velocity materials. The results show that the signal-to-noise ratios of detectors made of these materials could be improved by a factor of 15 to 100 at 4 K as compared to current detectors with aluminum antennas. A spherical gravitational wave antenna is very promising for gravitational wave astronomy because of its large cross-section, isotropic sky coverage, and the capability it can provide for determining the wave direction. In this dissertation several aspects of spherical detectors, including the eigenfunctions and eigenfrequencies of the normal-modes of an elastic sphere, the energy cross-section, and the response functions that are used to obtain the noise-free solution to the inverse problem are discussed. Using the maximum likelihood estimation method the inverse problem in the presence of noise is solved. We also determine the false-alarm probability and the detection probability for a network of spherical detectors and estimate the detectable event rates for supernovae core collapses and binary coalescences. Six identical cylindrical detectors, with a suitable arrangement of relative orientations, can form a detector network with detection sensitivity independent of the wave direction and polarization. This detector network, like a spherical detector, can provide a solution to the inverse problem in the presence of noise. The estimation errors for this network, similar to those for a spherical detector, are also discussed.
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