Optimization of parameters and the ultimate sensitivity of interferometric detectors of gravitational waves
| Autor: | Yu. V. Troitskiĭ |
|---|---|
| Rok vydání: | 2001 |
| Předmět: |
Physics
Interferometric visibility Atom interferometer Gravitational-wave observatory business.industry Gravitational wave Astrophysics::Instrumentation and Methods for Astrophysics Physics::Optics Michelson interferometer Atomic and Molecular Physics and Optics Electronic Optical and Magnetic Materials law.invention Interferometry Optics law Astronomical interferometer Laser power scaling business |
| Zdroj: | Optics and Spectroscopy. 90:250-255 |
| ISSN: | 1562-6911 0030-400X |
| DOI: | 10.1134/1.1351582 |
| Popis: | The signal-to-shot-noise ratio is calculated for three types of laser interferometers used in gravitational wave detectors: for two types of Fabry-Perot interferometers (with direct reading of the output signal and with the modulation technique used for outcoupling the signal) and for the Michelson interferometer with Fabry-Perot arms. It is shown that the signal-to-noise ratio can be substantially increased by using “supermirrors” with losses of the order of 10 −6. It is very important, in this case, to properly choose the mirror transmittance, because, otherwise, the sensitivity inevitably decreases by orders of magnitude and the requirements of lasers become more stringent. The efforts to increase the signal-to-noise ratio by increasing the power are limited either by an insufficient laser power or by the overheating of interferometer mirrors. Our estimates show that the present-day technical level with laser power of about 1 W provides sufficient sensitivity for detecting gravitational waves. |
| Databáze: | OpenAIRE |
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