thermal noise in gw detectors how much can an object be at rest on earth?
DESCRIPTION
Thermal noise in GW detectors How much can an object be at rest on Earth?. Geppo Cagnoli [email protected] INFN - Firenze University of Glasgow ITIS Citta’ di Castello UTB - Physics & Astronomy - 16 Sept. 2009. Fixing the problem. Earth is not an inertial reference frame - PowerPoint PPT PresentationTRANSCRIPT
Thermal noise in GW detectors
How much can an object be at rest on Earth?
Geppo [email protected]
INFN - FirenzeUniversity of GlasgowITIS Citta’ di Castello
UTB - Physics & Astronomy - 16 Sept. 2009
16 Sept 2009 UTB - Geppo Cagnoli - Thermal noise in GW detectors 2 of 22
Fixing the problem
• Earth is not an inertial reference frame
• Tidal effects
• Geological movements
Time scale or frequency rangehas to be defined
1Hz to 10 kHz
16 Sept 2009 UTB - Geppo Cagnoli - Thermal noise in GW detectors 3 of 22
Limiting the range
We could live the object on a tablebut
the Earth is noisy
Sfxx ( ). 012
mHz
Uncertainty PrincipleEt = h / 4
For a 10 kg mass:
Sfxx ( ) 10 18 m
Hz
1.E-22
1.E-18
1.E-14
1.E-10
1.E-06
1.E+00 1.E+01 1.E+02 1.E+03 1.E+04
[Hz]
m /
sqrt
(Hz)
10 orders of magnitude
16 Sept 2009 UTB - Geppo Cagnoli - Thermal noise in GW detectors 4 of 22
Mechanical Filteringof the Seismic Noise
Connectedto ground
Object
x
yA simple pendulumprovides a goodfiltering above theresonant frequency
20ff
)f(y)f(x
Possible improvements
• Use a spring to filter the vertical noise too
• With a multiple pendulum configuration is possible to fill the10 orders of magnitude
• We could use some damper to reduce the resonant peaks
16 Sept 2009 UTB - Geppo Cagnoli - Thermal noise in GW detectors 5 of 22
Virgo Superattenuator
THE REFERENCE POINT !!
16 Sept 2009 UTB - Geppo Cagnoli - Thermal noise in GW detectors 6 of 22
The Brownian motion
A challenge for the audience: how would you establish that this endless motion is not due to the activity of living organisms?
2 micron particles in water (left) and in concentrated DNA solution (right), 4 s of data
http://www.deas.harvard.edu/projects/weitzlab/research/brownian.html
Botanist Robert Brown, (1773-1858)
In 1832 the botanist Robert Brown observed a random motion of pollen and dust grains suspended in water
16 Sept 2009 UTB - Geppo Cagnoli - Thermal noise in GW detectors 7 of 22
Einstein’s Insight of 1905:A Way to Measure kB
average
diffusivity of big particle
Boltzmann's constant
absolute temperature (in kelvin)
3.14159...
viscosity of fluid
2
6
D
k
T
d Dt
kTD
r
radius of big particle r
Einstein’s specific prediction: in pure water at temperature 17o C (290 K or 63o F), a particle of diameter 1 m will move an average horizontal distance equal to 6 m in one minute.
16 Sept 2009 UTB - Geppo Cagnoli - Thermal noise in GW detectors 8 of 22
Is Einstein famous for Relativity?
16 Sept 2009 UTB - Geppo Cagnoli - Thermal noise in GW detectors 9 of 22
Random motion also in mechanical systems
R.K.PathriaStatistical MechanicsPergamon Press
Reducing the air pressure, the r.m.s.motion doesn’t change
butthe lower trace is almost monochromatic
whereas the higher is more random
It MUST vibrate ifthe equipartitiontheorem is right !
<E> = kT/2for each d.o.f.
16 Sept 2009 UTB - Geppo Cagnoli - Thermal noise in GW detectors 10 of 22
Non equilibrium thermodynamics
• Non isolated system shows uncorrelated fluctuations of volume and temperature
• Two independent fluctuating variables: T, V
TB
2
V
2B2
PV
TkVCTk
T
system
16 Sept 2009 UTB - Geppo Cagnoli - Thermal noise in GW detectors 11 of 22
Some comments
TB
2
V
2B2
PV
TkVCTk
T
• EASY TO JUSTIFY MECHANICAL VIBRATION FROM VOLUME FLUCTUATION
• NO SPECTRAL INFORMATION FROM THE PREVIOUS RELATIONS
• RESIDUAL GAS EFFECT IS HARD TO BE IMPLEMENTED
16 Sept 2009 UTB - Geppo Cagnoli - Thermal noise in GW detectors 12 of 22
The Fluctuation-Dissipation Theorem - 1
• H.B. Callen and T.A. Welton, Phys. Rev. 83, 34 (1951)
• R Kubo 1966 Rep. Prog. Phys. 29 255-284
• It applies to linear systems in thermal equilibrium
• It is used to predict the level of thermal noise of one observable x of the system
Linear system
X(t)F(t)
16 Sept 2009 UTB - Geppo Cagnoli - Thermal noise in GW detectors 13 of 22
The Fluctuation-DissipationTheorem - 2
• It gives the amplitude of the fluctuations of force Sff() that is shaking the system, at each angular frequency
• As seen in the experiments, the noise spectrum is shaped by the “friction”
() =SPEED
FORCE=
v()
F()
)(Tk4)(S Bff
Coefficient ofviscosity =
16 Sept 2009 UTB - Geppo Cagnoli - Thermal noise in GW detectors 14 of 22
The double approachto thermal noise
• Direct
– 2 variables are fluctuating
– Intuitive
– The spectrum is hard to extract
• Indirect
– Dissipation replaces fluctuation
– Not intuitive
– Extremely powerful for noise level prediction: is “easy” to measure ()
TB
2
V
2B2
PV
TkVCTk
T
)(Tk4)(S Bff
16 Sept 2009 UTB - Geppo Cagnoli - Thermal noise in GW detectors 15 of 22
Our system
• 20 to 40 kg silica mirror
• Suspended by 4 fibres
• Dielectric coatings applied on the front faces for maximizing or minimizing reflection
• The reference is the mass front face, where the laser beam senses the position
16 Sept 2009 UTB - Geppo Cagnoli - Thermal noise in GW detectors 16 of 22
Volume fluctuations in solids
• The volume fluctuations (as the thermal ones) need to fulfil the boundary conditions
• Perfect solids (crystals) vibrates at their resonant frequencies
• The real solids have defects that move or change driven by the finite temperature of the solid:
– The vibration has a continuous spectrum rather than a discrete one
• NO DIRECT METHOD APPROACH:
– Mechanical losses of materials are investigates and thermal noise level is worked out through FDT
16 Sept 2009 UTB - Geppo Cagnoli - Thermal noise in GW detectors 17 of 22
How to measure the mechanical loss
A method widely used is to detect the free decay of the excited resonances of the system
In order to know the frequency distribution of noise, the viscosity constant has to be measured at all the frequencies of interest
A0/eA0
( )0
2m
16 Sept 2009 UTB - Geppo Cagnoli - Thermal noise in GW detectors 18 of 22
Sample
Vacuumtank
Sapphirehalf sphere
A new sample holding systemGeNS Dr. Elisabetta Cesarini
16 Sept 2009 UTB - Geppo Cagnoli - Thermal noise in GW detectors 19 of 22
The most severe limit for IFOs:thermal noise from the coatings
• Alternate layers of transparent materials with different index of refraction
• Impedance mismatch andinterference produce highcoefficient of reflectivity
• Its structure is not compact as the substrate
• 10 m of coating produces morethermal noise than 10 cm of substrate
16 Sept 2009 UTB - Geppo Cagnoli - Thermal noise in GW detectors 20 of 22
Asymmetrical thermal fluctuations are responsible of thermoelastic noise on silica fibres (DIRECT APPROACH)
In linear thermoelastic effect thermal expansion coefficient transforms thermal fluctuations in strain fluctuations
= ·T
Thermoelastic noiseEffect on suspension fibres - 1
Fibres bend and then the suspendedmass is shaken. The effect is small butrelevant in GW detectors
Same kind of deformations occur in mirrors
16 Sept 2009 UTB - Geppo Cagnoli - Thermal noise in GW detectors 21 of 22
Thermoelastic noiseEffect on suspension fibres - 2
• The heat transfer sets a characteristic time scale that makes the noise spectrum frequency dependent, like:
Debye peak:
2max
2 ff
f
Nois
e o
r fr
icti
on
in
ten
sity
frequency
• Fused silica facts:— Low — Low — High strength
16 Sept 2009 UTB - Geppo Cagnoli - Thermal noise in GW detectors 22 of 22
Fused silica fibre productionand testing
• The CO2 laser pulling machine was developed in Glasgow
• The machine was financed by EGO as well as PPARC and in 2006 it was delivered to Pisa
• The machine was then adapted to the Virgo necessities and thanks to the excellent work of Dr. Matteo Lorenzini, Francesco Piergiovanni, Dr. Filippo Martelli, Virgo now has fused silica suspensions of high precision and strength