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          Institute: MPI für Gravitationsphysik     Collection: Laser Interferometry & Gravitational Wave Astronomy     Display Documents



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ID: 372285.0, MPI für Gravitationsphysik / Laser Interferometry & Gravitational Wave Astronomy
Mechanical aspects in interferometric gravity wave detectors
Authors:Winkler, Walter; Chen, J. M.; Danzmann, Karsten; Nelson, P. G.; Niebauer, T. M.; Rüdiger, Albrecht; Schilling, Roland; Strain, Kenneth A.; Schnupp, L.; Walther, H.; Hough, J.; Campbell, A. M.; Cantley, C. A.; Logan, J. E.; Meers, B. J.; Morrison, E.; Newton, G. P.; Robertson, D. I.; Robertson, N. A.; Rowan, S.; Skeldon, K. D.; Veitch, P. J.; Ward, H.; Welling, H.; Aufmuth, Peter; Kröpke, I.; Ristau, D.; Hall, J. E.; Bennett, J. R. J.; Corbett, I. F.; Edwards, B. W. H.; Elsey, R. J.; Greenhalgh, R. J. S.; Schutz, Bernard F.; Nicholson, D.; Shuttleworth, Justin R.; Ehlers, Jürgen; Kafka, P.; Schäfer, Gerhard; Braun, H.; Kose, V.
Publisher:Springer
Place of Publication:Berlin / Heidelberg
Date of Publication (YYYY-MM-DD):1992
Title of Proceedings:Relativistic gravity research : with emphasis on experiments and observations
Start Page:239
End Page:266
Title of Series:Lecture Notes in Physics
Volume (in Series):410
Name of Conference/Meeting:W.-E.-Heraeus-Seminar ; 81
Place of Conference/Meeting:Physikzentrum, Bad Honnef, Germany
(Start) Date of Conference/Meeting
 (YYYY-MM-DD):
1991-09-02
End Date of Conference/Meeting 
 (YYYY-MM-DD):
1991-09-06
Review Status:not specified
Audience:Not Specified
Abstract / Description:In order to measure the tiny effects of gravitational waves, strains in space (i.e. relative changes in distance) of as little as 10-21 or even less have to be detected, at frequencies ranging from 10011z to several kHz. Large laser interferometers are the most promising approach to reach such extreme sensitivities. This lsquostraightforwardrsquo road is, however, obstructed by a multitude of effects that cause (or fake) such fluctuations in distance. Among these are seismic motions, thermal vibrations of optical components, pressure fluctuations of the residual gas in the vacuum tubes, and fundamental effects such as Heisenberg's uncertainty relation.
What all of these noise sources have in common is that their effects can be reduced by the choice of sufficiently large arm lengths. This is what dictates the (very expensive) choice of arm lengths of 3 to 4 km in the currently proposed gravitational wave detectors (USA, D-GB, F-I, AUS, JAP).
External Publication Status:published
Document Type:Conference-Paper
Communicated by:Karsten Danzmann
Affiliations:MPI für Gravitationsphysik/Laser Interferometry & Gravitational Wave Astronomy
MPI für Gravitationsphysik/Teilinstitut Hannover
MPI für Gravitationsphysik/Astrophysical Relativity
MPI für Gravitationsphysik/Geometric Analysis and Gravitation
MPI für Gravitationsphysik/GEO 600
External Affiliations:Max-Planck-Institut für Quantenoptik, D-8046 Garching, Germany
Department of Physics and Astronomy, University of Wales College of Cardiff
Identifiers:ISSN:1616-6361
ISBN:978-3-540-56180-4
DOI:10.1007/3-540-56180-3_11
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