effects of laser linewidth on the back-action cooling of optomechanical resonators
DESCRIPTION
Effects of laser linewidth on the back-action cooling of optomechanical resonators. Gregory A. Phelps This work is sponsored by: UA NASA Space Grant, NSF, ARO, ONR. Introduction. Gravitational Wave Detection (LIGO) 4 kilometer interferometer. (Hartle, 339-342). - PowerPoint PPT PresentationTRANSCRIPT
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Effects of laser linewidth on the back-action cooling of
optomechanical resonators.
Gregory A. Phelps
This work is sponsored by:
UA NASA Space Grant, NSF, ARO, ONR
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Introduction
Gravitational Wave Detection (LIGO)• 4 kilometer interferometer
€
δx
L≈10−21 ⇒ δx ≈10−18
€
EGS =hΩm
2≈10−8eV
1000 times smaller than a proton!
€
TGS ≈ 0.0004K
• Quantum Mechanical ground state of a macroscopic object.
LIGO at Hanford [1]
(Hartle, 339-342)
[1] http://www.jb.man.ac.uk/research/pulsar/images/Ligo_hanford.jpg
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Optomechanical System
From T. Kippenberg and K. VahalaScience 321, 1172 (2008)
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Equations of Motion
Under-damped driven harmonic oscillator. Forcing terms are due to thermal motion of the mirror and the interaction with
the intra-cavity light field. Equations are derived from Quantum Mechanical Hamiltonian for the mirror
and light field.€
˙ ̇ x +Ωm
2Qm
˙ x + Ωm2x = α
2+ FL t( )
˙ α = i Δ + ωcavity
x
L
⎛
⎝ ⎜
⎞
⎠ ⎟−
1
2
⎡
⎣ ⎢
⎤
⎦ ⎥α + iSe iφ t( )
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Thermal and Laser Noise
Thermal Noise:
€
FL t( ) = 0
FL t( )FL s( ) =2ΩmkbT
MQm
δ t − s( )
€
φ t( ) = 0
φ t( )φ s( ) =1
2τe− t−s /τ
Laser Noise (Frequency):
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Monte Carlo Methods/Simulations
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Temperature vs. Linewidth
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Conclusions
The opto-mechanical system can be modeled as a damped, driven harmonic oscillator.
The final temperature of the mirror is linearly dependent on the linewidth of the laser, for small linewidth.
Laser noise places a limit on the temperatures attainable. Constructing the system to have certain parameters can help to
overcome laser noise. Feedback systems in the laser can reduce the laser noise.
These sources of noise place a limitation on the sensitivity of the interferometer at LIGO.
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Acknowledgments
I would like to thank my advisor Pierre Meystre, Dan Goldbaum, Swati Singh, Ewan Wright for our lengthy discussions and their helpful insights.
This work is supported by the University of Arizona/NASA Space Grant, NSF, ARO, and ONR.
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References
Hartle, James. GRAVITY, An Introduction to Einstein's General Relativity. 1st ed. 1. San Francisco: Addison Wesley, 2003. 339-342. Print.