testing general relativity in fermilab: sergei kopeikin - university of missouri adrian melissinos -...
TRANSCRIPT
Testing General Relativity in Fermilab:
Sergei Kopeikin - University of Missouri
Adrian Melissinos - University of Rochester
Nickolai Andreev - Fermilab
Nikolai Mokhov - Fermilab
Sergei Striganov - Fermilab
Working Sub-Group: Relativistic Gravity in Particle Physics
Gravity regime normally tested:• weak field (U << c²)• slow motion (v << c)
Gravity regime for LIGO:• strong field (U ≤ c²)• fast motion (v c)• Problem – identification of signal with the source
Gravity regime for Fermilab:• Weak field (U << c²)• Fast motion (v c)• Advantage – experimental parameters are
controlled
• Understanding of mass: is the inertial and gravitational masses of the particles the same?
• Understanding of anti-matter: does anti-matter attract or repeal?
• Understanding mechanism of the spontaneous violation of the Lorentz symmetry
• Possible window to extra dimensions • Understanding of various mechnisms for extention
of the standard model
Why to Measure Gravity at Microscopic Scale?
Metric perturbation induced at a distance b from the beam,
< h > ~ (4G/c2) γm (N/2πR) ln(2γ)
Bunch length cτB >> b, γ = E/m, R = Tevatron radius, N = circulating protons
If G = GN h ~ 10-40 hopeless !!
If gravity becomes “strong” at this highly relativistic velocity
G = Gs = GN(MP/MS)2
For Ms < MP/108 = 108 TeV h > 10-24
The effect is detectable in 100 s of integration !
• Noise and false signal issues could be severe• A 1986 Fermilab expt used a s.c. microwave parametric
converter and set a limit MS > 106 TeV
A. Melissinos: Fermilab Colloquim, Nov 14, 2007
Wish to measure the gravitational field of the Tevatron beam!
Modulate the proton beam to λ = 2L ~ 30 m. At some distance from the
beam line, install a high finesse Fabry-Perot cavity of length L ~ 15 m
Any perturbation at 10 MHz of dimensionless amplitude h
populates the excited modes and gives rise to 10 MHz sidebands
Ps = P0 (h Q)2
For reasonable values, Q = 1014 , P0 = 10 W and recording one photon per second, one can detect
h ~ 10-24
Optical Cavity
15 m
30 mFilled beam buckets
The cavity has excited modes spaced at the “free spectral range”
f = c/2L = 10 MHz
A. Melissinos: Fermilab Colloquim, Nov 14, 2007
Laser Parametric Converter as Gravity Detector
The ultra-relativistic force of gravity in Tevatron
• The bunch consists of N=3×10¹¹ protons • Ultra-relativistic speed = large Lorentz factor
=1000 • Synchrotron character of the force = beaming
factor gives additional Lorentz factors• Spectral density of the gravity force grows as a
power law as frequency decreases• The gravity force is a sequence of pulses (45000
“pushes” per second 36 bunches =1,620,000)
Numerical estimate of the gravity force
mass 2mass 19 2
0
charge mass2 2 3charge 23 20
2 3/20
40 0
44.4 10 cm/sec
6.8 10 cm/sec( )
at the fundamental beam-revolution frequency 2 2.3 10 rad/sec,
grav pgrav
grav gravgrav
F GNma
M d
F FNrGN ea
M Mc d d
d
3
12
160
10 cm - minimal distance between the beam and detector,
= 1 km - radius of Tevatron,
=10 - the Lorentz factor,
10 - number of protons in bunch,
1.54 10 cm - radius of proton.
N
r
Laser Interferometer for Gravity Physics at Tevatron
16 18(10 10 ) cm/L Hz
L = 999.5 md = 0.07 mL = 16.7 m
Current technology of LIGO coordinate meters allows us to measure position of test mass with an
error
+d
Probe mass
Proton’s beam
Probe mass
16 18
3
13
15
cm (10 10 )
For the detector frequency 10 Hz
4.4 10 cm
3.2 10 cm
m
LHz
x
L
Problems to solve:
Theory – solving gravity field equations without a small parameter v/c (the post-Newtonian approximations fails). Synergy with LIGO. Re-consider LIGO expectations – the gravity signal is anisotropic (synchrotron gravitational radiation)
Experiment – shielding against the background noise and parasitic signals
Thank You!