Search results
Results from the WOW.Com Content Network
Adhikari has been involved in the construction and design of gravitational-wave detectors since 1997. [19] He started working on laser interferometers as a graduate student at MIT, with a particular focus on the variety of noise sources, feedback loops and subsystems, [20] [21] and helped to reduce the noise in all 3 of the LIGO interferometers while working on the Livingston interferometer.
A laser is divided into two beams by a beam splitter tilted by 45 degrees. The two beams propagate in the two perpendicular arms of the interferometer, are reflected by mirrors located at the end of the arms, and recombine on the beam splitter, generating interferences which are detected by a photodiode. An incoming gravitational wave changes ...
During the Initial and Enhanced LIGO phases, a half-length interferometer operated in parallel with the main interferometer. For this 2 km interferometer, the Fabry–Pérot arm cavities had the same optical finesse, and, thus, half the storage time as the 4 km interferometers. With half the storage time, the theoretical strain sensitivity was ...
From 1987 to 1994 he served as the director and principal investigator of the Caltech-MIT Laser Interferometer Gravitational-Wave Observatory project, becoming a co-recipient of the 2016 Special Breakthrough Prize in Fundamental Physics. [2] In 1992, he was elected a Fellow of the American Association for the Advancement of Science. [7]
The original application of the N-slit laser interferometer was interferometric imaging. [ 6 ] [ 10 ] [ 14 ] In particular, the one dimensionally expanded laser beam (with a cross section 25-50 mm wide by 10-25 μm high) was used to illuminate imaging surfaces (such as silver-halide films) to measure the microscopic density of the illuminated ...
Print/export Download as PDF; Printable version; In other projects ... Pages in category "Interferometers" The following 45 pages are in this category, out of 45 ...
The Laser Interferometer Gravitational-Wave Observatory (LIGO) uses two 4-km Michelson–Fabry–Pérot interferometers for the detection of gravitational waves. [38] In this application, the Fabry–Pérot cavity is used to store photons for almost a millisecond while they bounce up and down between the mirrors.
Bath interferometer (common path) Cyclic interferometer; Diffraction-grating interferometer (white light) Double-slit interferometer; Dual-polarization interferometry; Fabry–Pérot interferometer; Fizeau interferometer; Fourier-transform interferometer; Fresnel interferometer (e.g. Fresnel biprism, Fresnel mirror or Lloyd's mirror)