Cornell2

Views:
 
Category: Entertainment
     
 

Presentation Description

No description available.

Comments

Presentation Transcript

A new family of flat-topped beams interesting for future LIGO interferometers: 

A new family of flat-topped beams interesting for future LIGO interferometers Mihai Bondarescu California Institute of Technology

Collaborators and Consultants: 

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)

Slide3: 


International Network of Interferometric Detectors: 

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

LIGO : 

LIGO Collaboration of ~350 scientists at ~30 institutions Hanford Washington Slide adapted from a talk by Kip

Slide6: 

Livingston, Louisiana Slide adapted from a talk by Kip

LIGO’s International Partners: 

LIGO’s International Partners Slide adapted from a talk by Kip

How a LIGO Interferometer Works: 

How a LIGO Interferometer Works Fabry-Perot Cavity Fabry-Perot Cavity Beam Splitter Slide adapted from a talk by Kip

Slide9: 

Slide adapted from Rejean J Dupuis talk from http://www.ligo.org/results/

Noise in LIGO : 

Noise in LIGO Adopted from Kip’s Talk (LIGO-G030137-00-Z)

What is Thermoelastic Noise and How to Reduce It?: 

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

What is Thermoelastic Noise and How to Reduce It?: 

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

Building a MESA beam: 

Building a MESA beam Minimal Gaussian

Building a MESA beam: 

Building a MESA beam Minimal Gaussian

Building a MESA beam: 

Building a MESA beam Minimal Gaussian

Building a MESA beam: 

Building a MESA beam Minimal Gaussians

Building a MESA beam: 

Building a MESA beam Mesa

Flat and Concentric Configurations: 

Flat and Concentric Configurations (O’Shaugnessy, Thorne) (Bondarescu, Kazarian,Savov)

Flat and Concentric Configurations: 

Flat and Concentric Configurations (O’Shaugnessy, Thorne) (Bondarescu, Kazarian,Savov)

My proposal: 

My proposal Mirror Overlap minimal Gaussians centered on these lines

What’s different?: 

What’s different? Surfaces of constant phase Mimimal Gausian’s axis

What’s different?: 

What’s different? Flat Mirrors Confocal Mirros D

Mesa Beams Comparison: 

Mesa Beams Comparison

Mexican-Hat Mirrors’ Corrections: 

Mexican-Hat Mirrors’ Corrections

Tilt Instability: 

Tilt Instability Reduce Thermoelastic Noise Evaluate Tilt Instability for New Mirrors’ Shapes Compare to Conventional Spherical Mirrors Fabry-Perot Cavity

The Eigenvalue Problem: 

The Eigenvalue Problem

Mesa Beam Profiles: 

Mesa Beam Profiles

Flat-Concentric MB Comparison: 

Flat-Concentric MB Comparison Eigenstates Comparison Eigenvalues Comparison

Again Flat-Concentric Configurations Relation: 

Again Flat-Concentric Configurations Relation (Yanbei Chen) G=1-L/R

Results and Conclusions: 

Results and Conclusions Thermoelastic Noise (O,Shaughnessy, Strigin, Vyatchanin) Tilt Instability (Mode Mixing) Nearly Flat Concentric Duality (in Progress)

authorStream Live Help