Thermal noise from optical coatings in gravitational wave detectors

被引:111
作者
Harry, GM [1 ]
Armandula, H
Black, E
Crooks, DRM
Cagnoli, G
Hough, J
Murray, P
Reid, S
Rowan, S
Sneddon, P
Fejer, MM
Route, R
Penn, SD
机构
[1] LIGO Lab, Cambridge, MA 01239 USA
[2] MIT, Cambridge, MA 01239 USA
[3] CALTECH, Pasadena, CA 91125 USA
[4] Univ Glasgow, Dept Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland
[5] Stanford Univ, Edward L Ginzton Lab, Stanford, CA 94305 USA
[6] Hobart & William Smith Coll, Dept Phys, Geneva, NY 14456 USA
关键词
D O I
10.1364/AO.45.001569
中图分类号
O43 [光学];
学科分类号
070207 ; 0803 ;
摘要
Gravitational waves are a prediction of Einstein's general theory of relativity. These waves are created by massive objects, like neutron stars or black holes, oscillating at speeds appreciable to the speed of light. The detectable effect on the Earth of these waves is extremely small, however, creating strains of the order of 10(-21). There are a number of basic physics experiments around the world designed to detect these waves by using interferometers with very long arms, up to 4 km in length. The next-generation interferometers are currently being designed, and the thermal noise in the mirrors will set the sensitivity over much of the usable bandwidth. Thermal noise arising from mechanical loss in the optical coatings put on the mirrors will be a significant source of noise. Achieving higher sensitivity through lower mechanical loss coatings, while preserving the crucial optical and thermal properties, is an area of active research right now. (c) 2006 Optical Society of America
引用
收藏
页码:1569 / 1574
页数:6
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