introduction to gravitational wave detection
DESCRIPTION
Introduction to Gravitational Wave Detection. Ronald W. Hellings Montana State University. PTA Workshop Penn State 7/20/05. 2 free masses. space. motion in this dimension is meaningless. The masses track each other with lasers. What is a gravitational wave?. A 2-D analogy. - PowerPoint PPT PresentationTRANSCRIPT
Introduction to
Gravitational Wave Detection
Ronald W. HellingsMontana State University
PTA WorkshopPenn State7/20/05
space
What is a gravitational wave?
• A 2-D analogy
motion in thisdimension ismeaningless
2 free masses
The masses trackeach other with lasers
The gravitational wave is a wave of curvature
each slice is a section ofan arc of constant radius
the free masses remain fixed at their coordinate points
As a gravitational wave passes through the space...
while the distance between them
increases due to the extra space in the curvature wave.
The laser signal has to cover more distance and is delayed
Why are gravitational waves called “a strain in space”?
points that are close have little space injected between them
points that arefurther away have morespace injected between them
h
Quadrupole Gravitational Waves
a ring of free test masses h+
mor
e sp
ace
less space
Quadrupole Gravitational Waves
a ring of free test masses
h
Let’s do the math
Geometry
Earth
plane wave
elliptical polarization
polarizationangle
propagationvector
n̂
pulsars
2 ( ) i jij ijds h dx dx
The Gravitational Wave Metric Tensor
ˆ ˆ( ) ( ) ( ) ( ) ( )ij ij ijh t h t h t n n
e.g. choose the z-axis along and the x-axis so = 0.n̂
1 0 0 0 1 0
0 1 0 and 1 0 0
0 0 0 0 0 0
Then
The path of the radio signal from the pulsar to the Earth is a null path, so
2 2
2 2
0
( ) 1i j
i jij ij ij
dt ds
dx dxdt h dx dx ds h
ds ds
1
2
e e e i j
ijp p p
dx dxdt ds h ds
ds ds Approximate
and integrate
1 1ˆ ˆ ˆ ˆ ( ) ( )
2 2
ei j i j
ij ij ijp
s s s h ds s s s H e H p
where ( ) ( )ij ijH t h t dt
1ˆ ˆˆ ˆ ( ) ( )
2i j
ij e e ij p ps s s H t H t n x n x
ˆ( ) ( )ij ijh t h t n xhij is a wave, so
reception occurs at t = t, x = 0 emission occurs at t = t s, ˆsx s
1ˆ ˆˆ ˆ (1 )
2i j
ij ijs s H t s H t n sso
The change in distance is proportional to the integral of the wave amplitude.
So let’s get an observable that is proportional to the wave
( ) 1ˆ ˆˆ ˆ (1 )
2i j
ij ijd
s s h t s h tdt
n s
Gravitational waves are proportional to the time derivative of pulsar arrival time residuals. But...
in the long wavelength limit (s<), ( ) ( ) ( )h t h t h t
( ) 1ˆ ˆˆ ˆ (1 )
2i j
ijd
s s sh tdt
n s
and
or 1ˆ ˆˆ ˆ (1 )
2i j
ijs s h t n s
LIGO
Low band of LISA
The Gravitational Wave Spectrum
Type Range Run Time Sources Instrument
HF 10 Hz 1000 Hz
compactstars
bars,LIGOs
MF 0.1 Hz 10Hz
10 Hz 10 mHz
1 nHz 10 Hz
10 nHz 0 Hz
? MAGGIE,lunar LIGO
LF binariesSMBHs
LISA
one per day
one per a few days
one per year
VLF
ULF
once in alifetime
cosmic astrophysics PTA
snapshotsonly
cosmicstructure
COBE, MAPPlanck, etc.
The Gravitational Wave Spectrum
Type Range Run Time Sources Instrument
HF 10 Hz 1000 Hz
compactstars
bars,LIGOs
MF 0.1 Hz 10Hz
10 Hz 10 mHz
1 nHz 10 Hz
10 nHz 0 Hz
? MAGGIE,lunar LIGO
LF binariesSMBHs
LISA
one per day
one per a few days
one per year
VLF
ULF
once in alifetime
cosmic astrophysics PTA
snapshotsonly
cosmicstructure
COBE, MAPPlanck, etc.
Long wavelength limit
Long and short regimes
Long and short regimes
Short wavelength only
( ) 1ˆ ˆˆ ˆ (1 )
2i j
ij ijd
s s h t s h tdt
n s
The Pulsar Limit
~1000 yearsnow
Every pulsar in every direction has correlated timingnoise due to this term. This allows a weighted correlationanalysis to optimally use data from multiple pulsars.
The correlated part of the timing noise
( )ˆ ˆ ˆ ˆ ˆ ˆ( ) ( ) ( )i j i j i j
ij ij ijd
s s h t s s h t s s h tdt
For the nth pulsar in the direction sn, this may be written
( )( ) ( ) ( )n
n n nd
h t h t n tdt
(This generalizes the result of Hellings & Downs, 1983, which assumed plane-polarized gravitational waves.)
The cross-correlation of data from 2 pulsars will produce
2
mn m n m n
m n
C h h h h
h h O nh
If are isotropic, and uncorrelated, then and h h
2mn mnC h O h h O nh
where 1
4mn m n m n d
But should be uncorrelated? and h h
IT DEPENDS ON THE SOURCE!
Needs
• Calculation of for plane polarization mn done
• Calculation of and for general polarizationmn mn
• Thought on sources of stochastic gravitational background