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April 24 2004GR fun @ Cornell1 A new family of flat-topped beams interesting for future LIGO interferometers Mihai Bondarescu California Institute of Technology
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April 24 2004GR fun @ Cornell2 Collaborators and Consultants K. Thorne (Caltech) Pavlin Savov (Caltech) Erika D’Ambrosio (Caltech) S. Vyatchanin (MSU, Moscow) S. Strigin (MSU, Moscow) R. O’Shaughnessy (NWU, Chicago) P. Kazarian (GCC)
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April 24 2004GR fun @ Cornell3
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April 24 2004GR fun @ Cornell4 International Network of Interferometric Detectors Network Required for: »Detection Confidence »Waveform Extraction »Direction by Triangulation LIGO Hanford, WA LIGO Livingston, LA GEO600 Hanover Germany TAMA300 Tokyo VIRGO Pisa, Italy Slide adapted from a talk by Kip
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April 24 2004GR fun @ Cornell5 LIGO Collaboration of ~350 scientists at ~30 institutions Hanford Washington 4 km 2 km Slide adapted from a talk by Kip
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April 24 2004GR fun @ Cornell6 Livingston, Louisiana 4 km Slide adapted from a talk by Kip
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April 24 2004GR fun @ Cornell7 LIGO’s International Partners VIRGO: Pisa, Italy [Italy/France] GEO600, Hanover Germany [UK, Germany] TAMA300, Tokyo [Japan] AIGO, Jin-Jin West Australia Slide adapted from a talk by Kip
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April 24 2004GR fun @ Cornell8 How a LIGO Interferometer Works Fabry-Perot Cavity Fabry-Perot Cavity Beam Splitter Slide adapted from a talk by Kip
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April 24 2004GR fun @ Cornell9 Slide adapted from Rejean J Dupuis talk from http://www.ligo.org/results/
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April 24 2004GR fun @ Cornell10 Noise in LIGO Adopted from Kip’s Talk (LIGO-G030137-00-Z)
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April 24 2004GR fun @ Cornell11 What is Thermoelastic Noise and How to Reduce It? Random Thermal Fluctuations (~0.5 mm) Hot Regions Expand; Cold Contract Beam Intensity Averages Over Mirror Surface Imperfect Averaging = Thermoelastic Noise Gaussian Beam Slide from a talk prepared by Pavlin Savov for PCGM
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April 24 2004GR fun @ Cornell12 What is Thermoelastic Noise and How to Reduce It? Random Thermal Fluctuations (~0.5 mm) Hot Regions Expand; Cold Contract Beam Intensity Averages Over Mirror Surface Imperfect Averaging = Thermoelastic Noise Mesa Beam Slide from a talk prepared by Pavlin Savov for PCGM
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April 24 2004GR fun @ Cornell13 Building a MESA beam Minimal Gaussian
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April 24 2004GR fun @ Cornell14 Building a MESA beam Minimal Gaussian
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April 24 2004GR fun @ Cornell15 Building a MESA beam Minimal Gaussian
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April 24 2004GR fun @ Cornell16 Building a MESA beam Minimal Gaussians
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April 24 2004GR fun @ Cornell17 Building a MESA beam Mesa
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April 24 2004GR fun @ Cornell18 Flat and Concentric Configurations (O’Shaugnessy, Thorne) (Bondarescu, Kazarian,Savov)
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April 24 2004GR fun @ Cornell19 Flat and Concentric Configurations (O’Shaugnessy, Thorne) (Bondarescu, Kazarian,Savov)
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April 24 2004GR fun @ Cornell20 My proposal Mirror Overlap minimal Gaussians centered on these lines
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April 24 2004GR fun @ Cornell21 What’s different? Surfaces of constant phase Mimimal Gausian’s axis
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April 24 2004GR fun @ Cornell22 What’s different? Flat Mirrors Confocal Mirros D
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April 24 2004GR fun @ Cornell23 Mesa Beams Comparison
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April 24 2004GR fun @ Cornell24 Mexican-Hat Mirrors’ Corrections
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April 24 2004GR fun @ Cornell25 Tilt Instability Reduce Thermoelastic Noise Evaluate Tilt Instability for New Mirrors’ Shapes Compare to Conventional Spherical Mirrors Fabry-Perot Cavity
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April 24 2004GR fun @ Cornell26 The Eigenvalue Problem
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April 24 2004GR fun @ Cornell27 Mesa Beam Profiles
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April 24 2004GR fun @ Cornell28 Flat-Concentric MB Comparison Eigenstates Comparison Eigenvalues Comparison
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April 24 2004GR fun @ Cornell29 Again Flat-Concentric Configurations Relation (Yanbei Chen) G=1-L/R
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April 24 2004GR fun @ Cornell30 Results and Conclusions Thermoelastic Noise ( O,Shaughnessy, Strigin, Vyatchanin ) Tilt Instability ( Mode Mixing ) Nearly Flat Concentric Duality ( in Progress )
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