Gravitational wave astrophysics · Gravitational wave astrophysics Denis Martynov, Massachusetts...
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Gravitational wave astrophysics
Denis Martynov,Massachusetts Institute of Technology
Baikal School on High Energy Physics and Astrophysics July 11, 2016
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LIGO Laboratory2
Overview
Different ways to observe the universe Plane wave solution to Einstein equations Gravitational waves detectors Signal processing in LIGO Astrophysical sources
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LIGO Laboratory3
Different ways to observe
• Electromagnetic waves
• Particles
• Gravitational waves
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Electromagnetic waves
Radiation Wavelength,m Sources Detectors
Gamma rays 10-12 pulsars, quasars, collision of compact objects Swift, Integral
X-rays 10-10 supernovae, binary stars, black holes NuSTAR, Chandra
Ultraviolet 10-8 young and old stars Astrosat, IRIS
Visible 10-6 stars, galaxies, planets Hubble, Kepler
Infrared 10-5 cool stars, nebular, redshifted galaxies JWST, SST
Microwave 10-2 CMB, compact sources COBE, WMAP
Radio 103 masers, gravitational lenses, early Universe VLBI, Spectr-R
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Particles
Particles Energy,eV Sources Detectors
Cosmic rays 109-1021 supernovae, active galactic nuclei Fermi, Veritas
Neutrinos 1011-1021 core of the stars, starburst galaxies IceCube, Baikal
Axion 10–6-100 possible component of cold dark matter CAST, Casper
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CLEO Conference, June 6, 2016LIGO-G1600884-v2
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Gravity as a geometrical propertyMetric g defines distance between all points of the spacetime
Once metric is known, geodesic (‘free-fall’) equations read
ds
2 =X
uv
guv(x, t)dxudx
vx
u
x
v
ds
d
2x
u
d⌧
2+ �u
k,vdx
k
d⌧
dx
v
d⌧
= 0, where
�uk,v =
1
2g
um
✓@gmk
@x
v+
@gmv
@x
k� @gkv
@x
m
◆
are Christoffel symbols.
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Einstein equationsconnect spacetime metric with mass-energy distribution
Rik = �8⇡G
c4(Tik � 1
2gikT
mm)
is the Ricci tensor;is the energy-momentum tensor.
Rik(gik)
Tik
Rik = (@�l
jk
@x
l� @�l
il
@x
k+ �l
ik�mlm � �m
il �lkm)
Ricci tensor is a function of the metric tensor
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Plane wave solutionIn the weak field regime the space-time is almost flat
The largest contribution to gravitational wave radiation comes from the quadruple moment I
huv(t) =2G
rc4Iuv(t�
r
c)
guv = diag(1,�1,�1,�1) + huv, huv ⌧ 1
Einstein equations can be simplified to ⇤huv = 0
hij =
0
BB@
0 0 0 0
0 �h+ h⇥ 0
0 h⇥ h+ 0
0 0 0 0
1
CCA cos(!t� kz)
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Gravitational waves
Time
Metric g defines distance between all points of the spacetimeds
2 =X
uv
guv(x, t)dxudx
v
Distance between particles fluctuates together with strain
�L = h+L
10
In this particular example in the figure h=1/5LIGO target sensitivity is h ~ 3e-24
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Michelson interferometer (LIGO design)
measures differential length of two arms using the detector at the antisymmetric port
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Network of antennas
12
LIGO Livingston
LIGO Hanford
Virgo, Italy
Kagra, Japan
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Network of antennas
13
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4 km
100 kW
1064 nm
Laser
22W800W
85mW
25mW
LIGO Laboratory14
Optical configuration
h =�L
L
10Hz < f < 10 kHz
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Advanced LIGO Timeline
Year Occasion
2004 Advanced LIGO approved
2008 Start of Advanced LIGO construction
2011-2014 Advanced LIGO installation and testing
2013-2015 Commissioning of Advanced LIGO
2015-2016 First science run of Advanced LIGO
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LIGO Laboratory16
Some of the Fundamental Questions That Gravitational Waves Can Address
Fundamental Physics» Is General Relativity the correct theory of gravity?» How does matter behave under extreme conditions?» Are black holes truly bald?
Astrophysics, Astronomy, Cosmology» Do compact binary mergers cause GRBs?» What is the supernova mechanism in core-collapse of massive stars?» How many low mass black holes are there in the universe?» Do intermediate mass black holes exist?» How bumpy are neutron stars?» Is there a primordial gravitational-wave residue?» Can we observe populations of weak gravitational wave sources?» Can binary inspirals be used as “standard sirens” to measure the local Hubble
parameter?
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LIGO Laboratory17
Signal processing in LIGO
We need to separate signal from noise:
1. power spectrum density 2. coherence tools 3. waveform matching
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Gravitational wave signal
0 0.02 0.04 0.06 0.08 0.1Time, sec
-3
-2
-1
0
1
2
3
Ampl
itude
noise+signalsignal * 10
101 102 103
Frequency, Hz
0.02
0.04
0.06
0.08
0.1
0.12
0.14
0.16
0.18
0.2
Ampl
itude
spe
crum
den
sity
, 1 /
Hz1/
2 noise+signal
In the time domain
Units:
h(t) = hgw(t) + hn(t)
[h(t)] = 1
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Gravitational wave signalIn the frequency domain
Units:
0 0.02 0.04 0.06 0.08 0.1Time, sec
-3
-2
-1
0
1
2
3
Ampl
itude
noise+signalsignal * 10
101 102 103
Frequency, Hz
0.02
0.04
0.06
0.08
0.1
0.12
0.14
0.16
0.18
0.2
Ampl
itude
spe
crum
den
sity
, 1 /
Hz1/
2 noise+signal
S(!) =
Z +1
�1< h(t)h(t+ ⌧) > e�i!⌧d⌧
h(!1�!2) =1
⇡
Z !2
!1
S(!)d!
[h(!)] =1pHz
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LIGO Laboratory20
Past, current and goal LIGO sensitivities
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LIGO Laboratory21
Excess power in the signal
Monitor signal in different frequency bands over time
But! Need to be careful and separate GW signal from internal instrument transients.
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LIGO Laboratory22
Coherence between the two instruments
Two interferometers measure gravitational waves and noise. GW signal is the same while noise is independent.
C(!) =S12S⇤
12
S11S22
where is the cross-power spectrum.S12(!)
S12(!) =
Z +1
�1< h1(t)h2(t+ ⌧) > e�i!⌧d⌧
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LIGO Laboratory23
Waveform matching
In the case we know what to expect:
where is the expected gravitational wave signal, and is the measured signal.
SNR ⇠Z T
0h(t)htl(t)dt
htl(t)h(t)
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LIGO Laboratory24
Harvesting astrophysical sources
We expect signals from
1. Binary compact objects (waveforms are known) • black hole - black hole • neutron star - black hole • neutron star - neutron star
2. Bursts • supernovae • gamma ray bursts
3. Stochastic background
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LIGO Laboratory25
Compact objects in LIGO: neutron stars and black holes
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LIGO Laboratory26
Neutron stars• Gravitational field at the surface of the neutron star
is 2*1011 times higher than on Earth
• Gravitational field acts as a gravitational lens and normally invisible parts of the neutron star become visible
• The inside temperature of a newly formed neutron star is 1011-1012K
• Equation of state of neutron stars is still unknown, radius is ~10 km
Neutron Star Formation
Image credit: NASA
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LIGO Laboratory27
Merger of compact objects
• Waveforms are computed using the general theory of relativity
• It is possible to distinguish masses and spins of neutron stars and black holes
• Limits on the speed of gravitational waves can be set
• Sky localization allows us to produce population estimates
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Merger of compact objects
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LIGO Laboratory29
GW150914 (BH-BH merger)
4 x 10-18 m
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LIGO Laboratory30
GW150914 (BH-BH merger)
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CLEO Conference, June 6, 2016LIGO-G1600884-v2
36 M◉
29 M◉
Simulation Slowed Down ~ 100X
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CLEO Conference, June 6, 2016LIGO-G1600884-v2
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LIGO Laboratory33
GW150914 parameters
Radiated Energy: M◉ Peak Luminosity: erg/s3−0.5+0.5 3.6−0.4
+0.5 × 1056
Hanford
Livingston
Abbott, et al. ,LIGO Scientific Collaboration and Virgo Collaboration, “Observation of Gravitational Waves from a Binary Black Hole Merger” Phys. Rev. Lett. 116, 061102 (2016)
Waveform is entirely consistent with General Relativity!
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LIGO Laboratory34
GW151226 (BH-BH merger)
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LIGO Laboratory35
GW151226 (BH-BH merger)
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LIGO Laboratory36
Population statistics
SNR ⇠ 1
R�
SNR ⇠ 1
R�⇥ exp(�R/R0)
Propagation laws considered in the literature
E. Calabrese et al. Testing Gravity with Gravitational Wave Source Counts. arXiv:1602.03883
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LIGO Laboratory37
Neutron star equation of state
Many models are listed in the literature LIGO can measured GW from the coalescence at
2-5kHz Prove of connection between BNS and GRB Where do metals come from?
Supernovae Binary neutron star mergers
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LIGO Laboratory38
Neutron star equation of state
500 700 1000 3000 500010�25
10�24
10�23
10�22
Frequency [Hz]
p S(f)
and
2p f|h(
f)|[
Hz�
1/2 ] Source Distance: 100 MpcaLIGO
VoyagerCryo Lungo
1.35 � 1.35 M� EOS 2H1.35 � 1.35 M� EOS HB
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LIGO Laboratory39
Physics of supernovae
GW burst from SN can help to understand explosion Signal is expected to be broadband (100Hz - 3kHz) New facilities are required for frequent detections
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Burst signals• Fast catastrophic processes in the
Universe
• Supernovae are potential sources of gravitational waves
Supernovae models give different results in
gravitational wave signal
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LIGO Laboratory41
Physics of supernovae
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Stochastic background
• Early universe
• Many unresolved inspirals
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LIGO Laboratory43
Summary of discussed topics
Generation of gravitational waves Signal processing in LIGO Astrophysical sources in the LIGO band
https://www.lsc-group.phys.uwm.edu/ppcomm/Papers.html
Source RangeBH-BH (30 Ms) 1Gpc
NS-NS 80MpcCore Colapse SN 10kpc-1Mpc
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CLEO Conference, June 6, 2016LIGO-G1600884-v2
GW150914 in popular culture
44
From The Guardian
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45
LIGO Scientific Collaboration
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LIGO Laboratory46
Continuous waves
Billion NS in our galaxy Strongest emitters are rapidly rotating NS (~1kHz) Theoretical ellipticity upper limit is 2e-5
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Continuous waves• Sources have a fairly constant
and well-defined frequency
• Examples are rotating neutron stars with a non-zero ellipticity
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Phase locked lasers (LISA design)
48
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Measure timing pulsars (Nanograv design)
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LIGO Laboratory50
Tests of alternative theories
Alternative gravity theories suggest extra dimensions, finite mass of graviton and etc
We can use EM from short GRB to set constrains on graviton mass and speed
Even counts and events
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LIGO Laboratory51
Alternative theories
10-1 100 101 102m2 (M-)
1016
1017
1018
1019
Bou
ndson
c=(c!
v g)
10-1 100 101 102m2 (M-)
10-23
10-22
10-21
Bou
ndson
mg
(eV
)
aLIGOVoyagerCryo Lungo
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LIGO Laboratory52
Continuous waves
Frequency (Hz)
Freq
uenc
y de
rivat
ive (H
z/s)
5 10 20 100 300 1000 3000
1e−1
31e−1
11e−0
91e−0
7 ε=1e−4 ε=1e−5 ε=1e−6
ε=1e−7
ε=1e−8
ε=1e−9
1 kpc
10 kpc
100 kpc
1 Mpc