1 kazuhiro yamamoto max-planck-institut fuer gravitationsphysik (albert-einstein-institut) institut...
TRANSCRIPT
![Page 1: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/1.jpg)
1
Kazuhiro Yamamoto
Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut)Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover
Gravitational wave and detectors
6 May 2010 @Università degli Studi di Trento, Trento, Italy
![Page 2: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/2.jpg)
2
6 May 2010 (Afternoon)
Gravitational wave and detectors
7 May 2010 (Morning)
Fundamental noise of interferometric gravitational wave detectors
![Page 3: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/3.jpg)
0.Abstract
3
I would like to explain …
(1) What is the gravitational wave ?
(2) Why do we want to detect gravitational wave directly ?
(3) How can we detect gravitational wave ?
(4) What kinds of detector are there ?
Did they provide scientific results ?
(5) What kinds of detector will there be ?
Will they be able to detect gravitational wave ?
![Page 4: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/4.jpg)
Contents
1. Gravitational wave
2. Aims of detection
3. Outlines of detectors
4. Recent results in observation
5. Summary
4
![Page 5: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/5.jpg)
1.Gravitational wave What is the gravitational wave ?
1915 A. Einstein : General theory of Relativity
“Gravitation is curvature of space-time.”
1916 A. Einstein : Prediction of gravitational wave
“ Gravitational wave is ripple of space-time.”
5
Wikipedia (A. Einstein, English)
A. Einstein, S. B. Preuss. Akad. Wiss. (1916) 688.
![Page 6: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/6.jpg)
6
http://spacefiles.blogspot.com
Gravitational wave
Speed is the same as that of light.
Transverse wave and two polarizations
1.Gravitational wave
![Page 7: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/7.jpg)
7
1.Gravitational wave Interaction of gravitational wave is too weak !
Artificial generation is impossible !
No experiment which corresponds to
Hertz experiment for electromagnetic wave
Astronomical events
Strain [(Change of length)/(Length)] : h ~ 10-21
(Hydrogen atom)/(Distance between Sun and Earth)
No direct detection until now
![Page 8: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/8.jpg)
8
1. Gravitational wave Indirect detection of gravitational wave
Binary pulsar
(R.A. Hulse and J.H. Taylor,
Astrophysical Journal 195 (1975) L51.)
Generation of gravitational wave
Energy emission
Change of period of binary
Observed change of period agrees with theoretical
prediction by radiation formula of gravitational wave.
J.H. Taylor et al., Nature 277 (1979) 437.
![Page 9: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/9.jpg)
9
1.Gravitational wave Recent result
J.M. Weisberg and J.H. Taylor, ASP Conference Series, 328 (2005) 25 (arXiv:astro-ph/0407149).
![Page 10: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/10.jpg)
10
1.Gravitational wave
Web site of Nobel foundation
![Page 11: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/11.jpg)
11
What is the motivation ?
Physics : Experimental tests for theory of gravitation
Astronomy : New window for astronomical observation
2.Aims of detection
No direct detection until now
![Page 12: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/12.jpg)
12
Physics : Experimental tests for theory of gravitation
(1) Speed : Alternative theories of gravitation predict the difference of speed between gravitational wave and light.
2.Aims of detection
C.M. Will, “Theory and experiment in gravitational physics”(1993) Cambridge University Press.
![Page 13: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/13.jpg)
13
2.Aims of detection (2) Polarization : Alternative theories of gravitation predict the 6 kinds of polarizations (General relativity : 2).
![Page 14: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/14.jpg)
14
2.Aims of detectionAstronomy : New window for observation
Gravitational wave astronomy
Gravitational wave sources
(1) Burst source
(2) Periodic source
(3) Stochastic source
![Page 15: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/15.jpg)
15
2.Aims of detection(1) Burst source : Supernova
Mechanism of the core-collapse SNe still unclear
Shock Revival mechanism(s) after the core bounce.
GWs generated by a SNe should bring information from the inner massive part of the process and could constrains on the core-collapse mechanisms.
M. Punturo, GWDAW Rome 2010
![Page 16: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/16.jpg)
16
2.Aims of detection(1) Burst source : Compact binary coalescence
Neutron star, Black hole
msec
chirp signalcoalescence
quasi-modeoscillation
-300Hz -1kHz
K. Kuroda Fujihara seminar (2009)
New standard candle for measurement of distance
Equation of state at high density, formation black hole
![Page 17: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/17.jpg)
17
2.Aims of detection(2) Periodic source : Pulsar
M. Punturo, GWDAW Rome 2010
Asymmetry of shape
Structure of interior
Rotating neutron star
![Page 18: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/18.jpg)
18
2.Aims of detection(3) Stochastic source (Background)
(a) Astronomical sources
Compact binary
(b) Cosmological sources (Early universe)
Cosmic Gravitational wave Background ?
Quantum fluctuation in inflation
Phase transition at early universe
(Grand Unified Theory(cosmic string), Electroweak, QCD, …)
![Page 19: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/19.jpg)
19
3.Outlines of detectorsThere are a lot of kinds of detectors !
Resonant detector
Interferometer (on Earth)
Interferometer (Space)
Doppler tracking
Pulsar timing
Polarization of cosmic microwave background
and so on …
Frequency range : 10-18 Hz – 108 Hz
![Page 20: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/20.jpg)
20
3.Outlines of detectorsResonant detector Gravitational wave excites resonant motion of elastic body.
Weber bar (most popular one)
Diameter : several tens cmLength : a few metersResonant frequency : about 1 kHz
“300 years of gravitation”(1987) Cambridge University PressFig. 9.8
![Page 21: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/21.jpg)
21
3.Outlines of detectorsJoseph Weber (1919-2000) Pioneer of gravitational wave detection
He is one of persons who proposed the concept of laser.
Other persons (C.H. Townes, N.G. Basov, A.M. Prokhorov) won Nobel prize in Physics (1964).
He started development of resonant detector. J. Weber, Physical Review 117 (1960) 306.
![Page 22: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/22.jpg)
22
3.Outlines of detectorsWeber event J. Weber, Physical Review Letters 22 (1969) 1302. “Evidence for discovery of gravitational radiation”
Coincidence between two detectors (Distance is 1000 km)
Direction of sources : Center of our galaxy
![Page 23: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/23.jpg)
23
3.Outlines of detectorsHowever, …
No experimentalists could confirm Weber event
even if they used detectors with better sensitivity !
We do not know what caused Weber event,
but gravitational wave did not.
Theorists pointed out that our galaxy disappears in
short period if center of galaxy emits so large energy.
![Page 24: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/24.jpg)
24
3.Outlines of detectorsFirst generation (room temperature)
University of Maryland (U.S.A.) …
Second generation (4 K)
Explorer (Italy, CERN), Allegro (U.S.A.),
Niobe (Australia), Crab (Japan) …
Third generation (< 100 mK)
Nautilus (Italy), Auriga (Italy),
Mini-Grail (Netherlands),
Mario Schenberg (Brazil) …
This is not a perfect list !
![Page 25: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/25.jpg)
25
3.Outlines of detectorsFirst generation (room temperature)
University of Maryland (U.S.A.) …
Second generation (4 K)
Explorer (Italy, CERN), Allegro (U.S.A.),
Niobe (Australia), Crab (Japan) …
Third generation (< 100 mK)
Nautilus (Italy), Auriga (Italy),
Mini-Grail (Netherlands),
Mario Schenberg (Brazil) …
![Page 26: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/26.jpg)
26
Exploler
G. Pizzella, ET first general meeting (2008)
![Page 27: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/27.jpg)
27
NAUTILUSINFN - LNF
G. Pizzella, ET first general meeting (2008)
![Page 28: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/28.jpg)
28
AURIGAPadova
3.Outlines of detectors
G. Pizzella, ET first general meeting (2008)
![Page 29: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/29.jpg)
29
3.Outlines of detectorsMario Schenberg
O.D. Aguiar et al., Classical and Quantum Gravity 25 (2008) 114042.
Mini-Grail
http://www.minigrail.nl/
About 3 kHz
![Page 30: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/30.jpg)
30
Old but original resonators in Japan (Not bar and sphere)
One of examples : Torsion detector (60 Hz)
Best upper limit of continuous gravitational wave from Crab pulsar h<2*10-22 (Until 2008)T. Suzuki, “Gravitational Wave Experiments”World Scientific p115 (1995).
3.Outlines of detectors
S. Kimura et al., Physics Letters A81 (1981) 302.
“Gravitational wave detection”Kyoto University Press (1998)Fig. 5-6. (Japanese)
![Page 31: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/31.jpg)
31
Interferometer (on Earth)Gravitational wave changes length difference of two arms.
3.Outlines of detectors
Frequency : 10 Hz – 10 kHz
![Page 32: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/32.jpg)
32
Brief early history of interferometer“300 years of gravitation”(1987) Cambridge University Press
Idea or suggestion F.A.E. Pirani (1956), Gertsenshtein and Pustovoit (1962), J. Weber (mid-1960’s)
Detailed design and feasibility study R. Weiss (1972)
First interferometric detector G.E. Moss, L.R. Miller, R.L. Forward, Applied Optics 10 (1971) 2495.
3.Outlines of detectors
![Page 33: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/33.jpg)
33
3.Outlines of detectors
All current interferometers have Fabry-Perot cavities.
![Page 34: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/34.jpg)
34
3.Outlines of detectorsFirst generation (Current)
LIGO (U.S.A.), VIRGO (Italy and France),
GEO (Germany and U.K.), TAMA (Japan), CLIO (Japan)
Second generation (Future)
Advanced LIGO, Advanced VIRGO,
AIGO(Australia), LCGT (Japan)
Third generation (Future)
Einstein Telescope (Europe)
![Page 35: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/35.jpg)
35
3.Outlines of detectorsSensitivity of interferometer
1st generation (LIGO,VIRGO)
2nd generation
3rd generation
10 times
10 times ?
![Page 36: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/36.jpg)
36
3.Outlines of detectorsLIGO (U.S.A.)
4 km, Hanford and Livingston (3000 km distance) (U.S.A.) S. Kawamura, Classical and Quantum Gravity 27 (2010) 084001.
![Page 37: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/37.jpg)
37
VIRGO (Italy and France)
3.Outlines of detectors
3 km, Pisa (Italy) S. Kawamura, Classical and Quantum Gravity 27 (2010) 084001.
![Page 38: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/38.jpg)
38
3.Outlines of detectorsGEO (Germany and U.K.)
600 m, Hannover (Germany) S. Kawamura, Classical and Quantum Gravity 27 (2010) 084001.
![Page 39: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/39.jpg)
39
3.Outlines of detectorsTAMA (Japan)
300 m, Tokyo (Japan) S. Kawamura, Classical and Quantum Gravity 27 (2010) 084001.
![Page 40: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/40.jpg)
40
3.Outlines of detectors
100 m, Kamioka (Japan) S. Kawamura, Classical and Quantum Gravity 27 (2010) 084001.
CLIO (Japan)
![Page 41: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/41.jpg)
41
3.Outlines of detectorsWhat will happen in future ?Before second generation …
GEO-HF (High Frequency)Upgrade of GEO600Observation : 2011-2015
Injection of squeezed light(smaller quantum vacuum fluctuation of light)
H. Lueck et al.,Journal of Physics: Conference Series Coming soon (arXiv:1004.0339).
Henning Vahlbruch et al.,Classical and Quantum Gravity 27 (2010) 084027.(GWIC thesis prize in 2008)
![Page 42: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/42.jpg)
42
3.Outlines of detectorsSecond generation Observation : 2015 ? – We can expect first detection !
Advanced LIGO, Advanced VIRGO
Upgrade of LIGO and VIRGO
AIGO (Australia)
Similar to Advanced LIGO
LCGT (Japan)
Cryogenic technique
Underground site (small seismic motion)
![Page 43: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/43.jpg)
43
3.Outlines of detectorsAIGO (Australia)
8 km, Perth (Australia) S. Kawamura, Classical and Quantum Gravity 27 (2010) 084001.
![Page 44: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/44.jpg)
44
Location of LCGTLCGT is planed to be built underground at Kamioka, where the prototype CLIO detector is placed.
By K. Kuroda (2009 May Fujihara seminar)
3 km, Kamioka (Japan)
![Page 45: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/45.jpg)
4545
3.Outlines of detectors
Prototype for LCGT (cryogenic technique, same underground site)
S. Kawamura, Classical and Quantum Gravity 27 (2010) 084001.
CLIO (Japan)
![Page 46: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/46.jpg)
46
3.Outlines of detectorsEinstein Telescope (Europe)
30 km vacuum tube in total
Cryogenic technique Underground site (small seismic motion)
Third generation Observation : 2025 ? –
![Page 47: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/47.jpg)
World wide network for GW astronomy
Adv. LIGO (under construction since 2008 )TAMA/CLIO
LCGT, Budget request
LIGO(I) Hanford
LIGO(I) Livingston
GEO 600
Virgo
AIGO (budget request)
Adv. Virgo (design)
ET (planed)
A network of detectors is indispensable to position the source.
LCGT
By K. Kuroda (2009 May Fujihara seminar)
GEO HF
![Page 48: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/48.jpg)
48
3.Outlines of detectors
M. Punturo et al., Classical and Quantum Gravity 27 (2010) 084007.
![Page 49: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/49.jpg)
49
4.Recent results in observation
Future interferometers can detect gravitational wave.Current interferometers have never detected !
However, current interferometers have already provided scientific results in astronomy and cosmology.
(1) Gamma ray burst
(2) Crab pulsar
(3) Stochastic background
![Page 50: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/50.jpg)
50
4.Recent results in observation
(1) Gamma ray burst
Gamma ray flashes with huge energy
1963 : Vela satellite (U.S.A.) found gamma ray burst.
R. Klebesadel et al., Astrophysical Journal 182 (1973) L85.
Nobody knows what they are and how much distances from Earth are.
Gamma ray bursts appear suddenly and disappear soon.
![Page 51: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/51.jpg)
51
4.Recent results in observation
(1) Gamma ray burst
Revolutions in 1997
BeppoSAX (Italy, Netherlands)Wikipedia, English
Identification of optical counterpartMeasurement of distance(order of billion light years !)
J. van Paradijs et al., Nature 386 (1997) 686.D.E. Reichart, Astrophysical Journal 495 (1998) L99.
However, central engine is still unknown.
![Page 52: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/52.jpg)
52
4.Recent results in observation
(1) Gamma ray burst
There are two categories.
Long gamma ray burst (more than 2 sec) Short gamma ray burst (less than 2 sec)
Central engine of short gamma ray burst
Compact binary coalescence ?
Neutron star – Neutron star, Black hole – Neutron star
If so, short gamma ray bursts generate gravitational wave !
![Page 53: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/53.jpg)
53
4.Recent results in observation
(1) Gamma ray burst
GRB070201 (1 February 2007) Direction : Andromeda galaxy (M31) 0.77Mpc (about 2 million light years)
Only LIGO interferometers were in operation.
B. Abbott et al., Astrophysical Journal 681 (2008) 1419.
![Page 54: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/54.jpg)
54
4.Recent results in observation
(1) Gamma ray burst
No signal was found !
This conclusion does not exclude current model in M31.However, some parameter regions are excluded.
If GRB070201 is in M31,
1 solar mass < m1 < 3 solar mass1 solar mass < m2 < 40 solar mass
This parameter region is excludedat >99% confidence.
B. Abbott et al., Astrophysical Journal 681 (2008) 1419.
![Page 55: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/55.jpg)
55
4.Recent results in observation
(2) Crab pulsar
Crab nebulaWikipedia, English
Rotating neutron star in Crab nebula (Supernova in 1054)
Spin down : Loss of rotation kinetic energyUpper limit of gravitational wave
Asymmetry of pulsar generates gravitational wave.
h<1.4*10-24
One of the largest upper limits in pulsars
![Page 56: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/56.jpg)
56
4.Recent results in observation
(2) Crab pulsar
Crab nebulaWikipedia, English
LIGO interferometers9 months data(Nov. 2005 - Aug. 2006)
h<2.7*10-25
No signal was found !
Upper limit of gravitational wave
Loss due to gravitational wave is less than 4% of total loss.
5 times smaller upper limit than that of spin-down
B. Abbott et al., Astrophysical Journal 683 (2008) L45.
![Page 57: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/57.jpg)
57
4.Recent results in observation
(3) Stochastic background
Cosmological stochastic background gravitational wavecould be generated in early universe.
After that, D, He, Li were generated (in first three minutesof universe). We can observe quantity of generated these elements. Their quantities depend on the speed of universe expansion.
If energy density of stochastic background gravitational wave was too much, speed of universe expansion was different from our expectation.
![Page 58: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/58.jpg)
58
4.Recent results in observation
(3) Stochastic background
So, energy density of stochastic gravitational wave background (around 100 Hz) must be 1.1*10-5 times smaller than average density of universe.
Big Bang nucleosynthesis
![Page 59: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/59.jpg)
59
4.Recent results in observation
(3) Stochastic background
LIGO interferometers : about 2 years data(Nov. 2005 - Sep. 2007)Correlation between 2 interferometers
No correlation was found !
So, energy density of stochastic gravitational wave background (around 100 Hz) must be 6.9*10-6 times smaller than average density of universe.
1.6 times smaller upper limit than that of Big Bang nucleosynthesisSome models of early universe are ruled out.
B.P. Abbott et al., Nature 460 (2009) 990.
![Page 60: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/60.jpg)
60
5.Summary Nobody has detected gravitational wave directly.
There are two kinds of motivation for direct detection;
physics and astronomy.
Resonant and interferometric detectors were constructed on Earth and are operated for observation.
Some scientific null results have already been obtained.
In near future, gravitational wave will be detected directly !
![Page 61: 1 Kazuhiro Yamamoto Max-Planck-Institut fuer Gravitationsphysik (Albert-Einstein-Institut) Institut fuer Gravitationsphysik, Leibniz Universitaet Hannover](https://reader038.vdocument.in/reader038/viewer/2022103122/56649ce15503460f949ac9f6/html5/thumbnails/61.jpg)
61
Thank you for your attention !
Vi ringrazio molto per la vostra attenzione !