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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. K. Thorne (Caltech) Pavlin Savov (Caltech) Erika D’Ambrosio (Caltech) S. Vyatchanin (MSU, Moscow) S. Strigin (MSU, Moscow)

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

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  1. A new family of flat-topped beams interesting for future LIGO interferometers Mihai Bondarescu California Institute of Technology GR fun @ Cornell

  2. 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) GR fun @ Cornell

  3. GR fun @ Cornell

  4. International Network of Interferometric Detectors • Network Required for: • Detection Confidence • Waveform Extraction • Direction by Triangulation TAMA300 Tokyo LIGO Hanford, WA GEO600 Hanover Germany VIRGO Pisa, Italy LIGO Livingston, LA GR fun @ Cornell Slide adapted from a talk by Kip

  5. 4 km 2 km LIGO Collaboration of ~350 scientists at ~30 institutions Hanford Washington GR fun @ Cornell Slide adapted from a talk by Kip

  6. 4 km Livingston, Louisiana GR fun @ Cornell Slide adapted from a talk by Kip

  7. GEO600, Hanover Germany [UK, Germany] VIRGO: Pisa, Italy [Italy/France] AIGO, Jin-Jin West Australia TAMA300, Tokyo [Japan] LIGO’s International Partners GR fun @ Cornell Slide adapted from a talk by Kip

  8. How a LIGO Interferometer Works Fabry-Perot Cavity Fabry-Perot Cavity Beam Splitter GR fun @ Cornell Slide adapted from a talk by Kip

  9. Slide adapted from Rejean J Dupuis talk from http://www.ligo.org/results/ GR fun @ Cornell

  10. Noise in LIGO Adopted from Kip’s Talk (LIGO-G030137-00-Z) GR fun @ Cornell

  11. 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 GR fun @ Cornell Slide from a talk prepared by Pavlin Savov for PCGM

  12. 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 GR fun @ Cornell Slide from a talk prepared by Pavlin Savov for PCGM

  13. Building a MESA beam Minimal Gaussian GR fun @ Cornell

  14. Building a MESA beam Minimal Gaussian GR fun @ Cornell

  15. Building a MESA beam Minimal Gaussian GR fun @ Cornell

  16. Building a MESA beam Minimal Gaussians GR fun @ Cornell

  17. Building a MESA beam Mesa GR fun @ Cornell

  18. Flat and Concentric Configurations (O’Shaugnessy, Thorne) (Bondarescu, Kazarian,Savov) GR fun @ Cornell

  19. Flat and Concentric Configurations (O’Shaugnessy, Thorne) (Bondarescu, Kazarian,Savov) GR fun @ Cornell

  20. My proposal Mirror Overlap minimal Gaussians centered on these lines GR fun @ Cornell

  21. What’s different? Mimimal Gausian’s axis Surfaces of constant phase GR fun @ Cornell

  22. What’s different? D Flat Mirrors Confocal Mirros GR fun @ Cornell

  23. Mesa Beams Comparison GR fun @ Cornell

  24. Mexican-Hat Mirrors’ Corrections GR fun @ Cornell

  25. Tilt Instability • Reduce Thermoelastic Noise • Evaluate Tilt Instability for New Mirrors’ Shapes • Compare to Conventional Spherical Mirrors Fabry-Perot Cavity GR fun @ Cornell

  26. The Eigenvalue Problem GR fun @ Cornell

  27. Mesa Beam Profiles GR fun @ Cornell

  28. Flat-Concentric MB Comparison Eigenstates Comparison Eigenvalues Comparison GR fun @ Cornell

  29. Again Flat-Concentric Configurations Relation G=1-L/R (Yanbei Chen) GR fun @ Cornell

  30. Results and Conclusions • Thermoelastic Noise (O,Shaughnessy, Strigin, Vyatchanin) • Tilt Instability (Mode Mixing) • Nearly Flat Concentric Duality (in Progress) GR fun @ Cornell

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