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Searches for very high frequency gravitational waves. Mike Cruise University of Birmingham. Signals from Neutron Stars. Signals from SMBH’s. LIGO , Virgo, LISA or pulsar timing are most likely to make the first detections. Why go to higher frequencies?. - PowerPoint PPT Presentation
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Mike Cruise
University of Birmingham
Searches for very high frequency gravitational waves
Signals from Neutron Stars
Signals from SMBH’s
LIGO , Virgo, LISA or pulsar timing are most likely to make the first detections
Why go to higher frequencies?
• Other branches of astronomy developed through mullti-frequency observations
• For frequencies >1 MHz– Cosmological signals from the Planck era.– KK mode oscillations in higher dimensions– EMW-plasma instabilities generate GW’s– Radiation from non-minimal coupling of the
EM and G fields
Very High Frequency detectors?
• The best upper limit at 100 MHz by Akutsu and Kawamura of ~10-17 was with an interferometer
• But Interferometer sensitivity worsens as• Minimum detectable EM signal in a 1 Hz
bandwidth ~ 10-20 W• Maximum EMW power ~ 10’s of MW
• ratio of min detectable signal ~ 10-27
max available energy
21
E or B
Pathways for coupling EM and Gravity
22
2 2 4
116
Gh T
c t c
F g g F
May contain EM Fields
Contain G potentials
How does a GW interact with a static EM Field?
• De Logi and Mickelson (1977)
Graviton
Virtual Photon( Static Magnetic Field )
Photon
3
228
c
LGBSpin states of g, B and
For one incoming graviton per second
What are the fluxes?
• Flux of photons is times the flux of gravitons
• EM Signal Power is
1
1622
2
hG
cFlux
22222
08
1cSinhKLBP
Early Universe
Brane Oscillations
• Seahra and Clarkson have calculated the GW emission in 5-D gravity when stellar mass black holes fall into a black hole
• Different from
the LF radiation from such
a system, there is also an
excitation of the
brane separation
itself
This is a Source which exists!
But maybe in a universe which doesn’t
Plasma-EMW instabilities
• Linearised field equations in terms of a small metric perturbation, h
• Interaction of EM Fields and EM Waves
42
2
22
2 161
c
Gh
tcx
FFFF
4
1
4
1
Increased charge density
contributes to stress energy
tensor
Tidal forces affect
chargedensity
Nucleosynthesis limit
Cosmological Models
Current DetectorsCurrent Detectors
Higher Energy Density
Cosmological Models
Current DetectorsGalactic centre
Shadow Brane
Galactic CentreVisible Brane
Two element interferometer
Nucleosynthesis limit
Statement
• The work presented here derives from many papers on EM-GW interactions published in properly peer reviewed journals since the 1970’s
• This work has no connection with (and does not support or endorse) ideas published by the HFGW group
Conclusion
• Very high frequency gravitational waves may allow us to observe the very early universe, violent astrophysical events or exciting areas of new physics
• Current detectors are now beginning observations of the Galactic Centre at GHz and Optical Frequencies
• A two element interferometer is being designed jointly by Birmingham and Jodrell Bank
Higher sensitivity
Gravitational Waves in Space
• measure the separation between three spacecraft using laser beams.
• Use a long baseline so that the movement is larger.
• Measure separation to 10 pm 10-11 m over 5 million km.
Other mechanisms
Bubble collisions Decay of Cosmic Strings
“ Conversion” process• Inverse Gertsenshtein Effect
• EMW signal ~ h2L2K2B2
• Same frequency and direction as GW
• Must ensure phase coherence of EMW and GW
BEMW
L
h
Lens+CCD
The Universe- and how we study it
• Everything we know about the Universe comes from studying electromagnetic waves ( Infra-red, X-rays, radio waves, etc) of different frequencies
• Different frequencies tell us about different temperature regimes
• But many of the problems in astrophysics are to do with mass, not temperature.
What can Gravity tell us?
Measuring the waves:Interferometer
Laser
Photodiode
Mass
Mass
The Largest Instrument Ever!
• Three spacecraft with laser beams between them in a solar orbit.
• The pattern rotates each year to scan the sky.
How does a GW affect an EMW?
• Amplitude• Direction• Frequency• Polarisation state
quiescentsig hEE ~
GW
EMFieldhEnergySig2~
lldp e
l
mm
MRkpcMxh 2/)5(
5.021 1.011
109
Other Inflation Theories
• Garcia -Bellido
What kind of Instrument?
• Interferometer sensitivity worsens as • Current best Upper Limit is by Akutsu,
Kawamura et al– 10-17 at 100 MHz
• So h ~ 10-23 at 1000Hz will be 10-20 at 1 GHz
221
min 14
8
1
P
ch
FLh
21
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