Abstract
Gravitational Waves (GWs) are perturbations of space-time which propagate at the speed of light. The existence of GWs is one of the greatest predictions of Einstein’s relativistic gravitational theory. GWs could carry information of the stars and the Universe which is inaccessible to electromagnetic radiation, cosmic rays and neutrinos. Direct detection of GWs is one of the most challenging and exciting subjects in physics. The efforts of direct detection of GWs started at the middle of last century. After near 50 years, large-scale laser interferometer GW detectors, such as LIGO in US and Virgo in Italy, were built in the beginning of this century. Although no GWs have been detected directly, these first generation detectors have reached their design sensitivities (which is unprecedented) anticipated more than 20 years ago. It is expected that not only direct detection of GWs will become possible after the advanced versions of LIGO/Virgo come online in around 2015, we will also be able to open a new window to observe our Universe and thus start the time of GW astronomy. We review the working principle, the performances and structures of the core parts of LIGO/Virgo alike GW interferometers, including the high sensitivity Michelson interferometer, the Fabry-Perot cavity, the power recycling system, the high power stabilized laser, the mode cleaner, the seismic attenuation system and the vacuum system.
Translated title of the contribution | The Laser Interferometer Gravitational Wave Detector |
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Original language | Chinese |
Pages (from-to) | 348-382 |
Number of pages | 35 |
Journal | Progress in Astronomy |
Volume | 32 |
Issue number | 3 |
DOIs | |
Publication status | Published - 2014 |
Externally published | Yes |
Keywords
- gravitational wave
- Laser
- interferometer
- Fabry-Perot cavity
- power recycling
- Seismic Attenuation