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Uncharted landscapes of the universerevealed by gravitational wave
observations
Symposium 2019 on the ITER/BA ActivitiesFusion Energy Forum of Japan
H He Li
6
質量数
エネ
ルギ
ー
核子の束縛エネルギー
鉄
7
How can we make these elements ?
Heavy nucleus
Strong Coulomb repulsion
ҧ𝜈𝑒
ⅇ−
ⅇ−
ҧ𝜈𝑒
β - decay
12Neutron Number
ProtonNumber
13
ProtonNumber
Neutron Number
14Neutron Number
ProtonNumber
15Neutron Number
ProtonNumber
16
Slow: s-process
Neutron Number
ProtonNumber
r-process• Rapid caputure of neutrons• Where does it happen ?
s-process• Slow capture of neutrons• Site: old stars
18
Gold
By Rob Lavinsky, iRocks.com – CC-BY-SA-3.0, CC BY-SA 3.0,
https://commons.wikimedia.org/w/index.php?curid=10465065
By Szaaman - https://commons.wikimedia.org/wiki/File:Gold_bullion_1.jpg, Public Domain,
https://commons.wikimedia.org/w/index.php?curid=35565318
Platinum
Uranium
20
Rapid: r-process
Neutron Number
ProtonNumber
22
Fe
SiONeCHe
H
23
SiONeCHe
H
Electron captureProton → Neutron
24
Neutron core
Shock wave
26
Neutron star
William Crochot -
http://science.nasa.gov/media/medialibrary/1999/02/25/ast05mar99_1a_resources/N_sctn2.jpg,
Public Domain, https://commons.wikimedia.org/w/index.php?curid=36335367
(C) KAGAYA
28
(C)NASA
Gravitational Wave
30
31
32
NASA/Goddard Space Flight Center/CI Lab
35
GW170817
PRL 119, 161101(2017)
ApJL 848:L12 (59pp), 2017
ApJL 848:L12 (59pp), 2017
NGC 4993
2017/8/18-19 2017/8/24-25
(C) NAOJ
39
Kilonova
Electro-MagneticRadiation
Neutron Number
ProtonNumber
Joel de Jesus Mendoza Temis arXiv:1409.6135
Neutron number
Ato
mic
Nu
mb
er
(C) M. Tanaka
43© T. Dietrich, S. Ossokine, H. Pfeiffer, A. Buonanno(Max Planck Institute for Gravitational Physics), BAM collaboration
44
arXiv:1710.05446 [astro-ph.HE]
1.7sec 𝑐𝐺𝑊 − 1 < 10−15
48
O1: 2015 Sept. 12 – 2016 Jan. 19
O2: 2016 Nov. 30 – 2017 Aug. 25(Virgo joined on 2017 Aug. 1)
O3: 2019 Apr. 1 - on going (until 2020 Apr. 30 )
49
O1: 2015 Sept. 12 – 2016 Jan. 19
O2: 2016 Nov. 30 – 2017 Aug. 25(Virgo joined on 2017 Aug. 1)
O3: 2019 Apr. 1 - on going (until 2020 Apr. 30 )
Black Hole mergers: 10
Neutron Star mergers: 1
50
O1: 2015 Sept. 12 – 2016 Jan. 19
O2: 2016 Nov. 30 – 2017 Aug. 25(Virgo joined on 2017 Aug. 1)
O3: 2019 Apr. 1 - on going (until 2020 Apr. 30 )
BH + BH: 23NS + NS: 3+BH + BS: 3+Mass Gap: 2
Black Hole mergers: 10
Neutron Star mergers: 1
51
O1: 2015 Sept. 12 – 2016 Jan. 19
O2: 2016 Nov. 30 – 2017 Aug. 25(Virgo joined on 2017 Aug. 1)
O3: 2019 Apr. 1 - on going (until 2020 Apr. 30 )
BH + BH: 23NS + NS: 3+BH + BS: 3+Mass Gap: 2
Black Hole mergers: 10
Neutron Star mergers: 1
Open Public Alert
53(C) NASA/SOHO
54(C)NASA
55By Philip D. Hall - Own work, CC BY-SA 3.0, https://commons.wikimedia.org/w/index.php?curid=51201468
56By NASA, The Hubble Heritage Team, STScI, AURA
57
Black Hole spin
GW waveform
doi:10.1038/nature23453
How do we detect gravitational waves ?
Gravitational Wave Amplitude
𝐿
Δ𝐿
Hydrogen
150 billion meters
150 billion meters
Hydrogen
Laser
Beam Splitter
Photo Detector
Michelson Interferometer
Laser
Photodetector
68
LIGO/T. Pyle
How far can we see ?
Multi-stage Vibration Isolation System
1
10000000000
Fused SilicaSapphire
Beamsplitter(370mm dia) during coating characterization iKAGRA TM (250mm dia) during figure measurement
77
Laser
PD
100W3km
Laser
PD
100W
Fabry-Perot Michelson
Laser
PD
100W
Power Recycling
Laser
PD
100W
Resonant Sideband Extraction(RSE)
KAGRA Interferometer
86
PRMPR2
PR3
SR3
SR2
SRM
ITMY
ETMY
ITMX ETMX
BS
Mode Cleaner
IMMT
IFI
BRT
BRT
Type-B
Type-Bp
Type-C
Others
Type-A (cryogenic)
OMC
OMMT
OFI
OST Output
Optics
Output Optics
PSL
3km
3km
Resonant Sideband Extraction (RSE)
87
Seismic
SuspensionThermal
The KAGRA Project
88
• Over 300 collaborators• Over 70 institutes from around the world
91
93
Pre-Isolator
Standard Filter
Bottom Filter
Intermediate Mass
Mirror
Recoil Mass
94
95
Type-A + Cryogenic Suspension
96
14m
Cryo-Payload
Type-A(room temp.)
Type-A Suspension Installation
97
99©Ray. Hori
101
LIGO/Axel Mellinger
104
LIGO + Virgo
(54 deg2)
LIGO + Virgo + KAGRA
(3.4 deg2)
106
Now
