general relativity in japan - 京都大学 › ~misao.sasaki › pdf › gr_in_japan.pdf ·...
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General Relativity in Japan – a historical perspective –
Misao Sasaki
YITP, Kyoto University
personal, highly biased
Ewha Womans U 23 December, 2015
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History: two main streams
Research Institute for Theoretical Physics, Hiroshima University
1944-1990
Research Institute for Fundamental Physics, Kyoto University
1953-(1990)
Yoshitaka Mimura wave geometry field theory classical & quantum gravity cosmology
Hideki Yukawa particle/nuclear theory solid state physics biophysics astrophysics + cosmology
Yukawa Institute for Theoretical Physics 1990 ~
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RITP Hiroshima University
Established in 1944, during the 2nd world war Mimura insisted “This institute won’t be any use for the war. It will be solely devoted to progress in basic science.” Ministry of Education and Culture (Monbu-sho) finally agreed: The purpose of the institute was announced as “ to perform integrated research on basic theories of physics”
This was possible thanks to Mimura’s extensive work on wave geometry which looked quite promising as an approach to quantum gravity.
wave geometry: 2ds g dx dx
ds dx
in short, fermionization of the geometry
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RITP Hiroshima University
The institute was destroyed by the atomic bomb.
After the war it was rebuilt in Takehara, a small town about 50 km from Hiroshima along the inland sea.
Until ~ 1970, RITP was the center of GR research in Japan.
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ADM formalism in expanding universe
H. Nariai and T. Kimura, PTP 28 (’62) 529.
Quantization of gravitational waves and mater fields in expanding universe
H. Nariai and T. Kimura,
PTP 29 (’63) 269; 29 (’63) 915; 31 (’64) 1138.
[cf. L. Parker, PRL 21 (’68) 562]
Discovery of gravitational anomaly
T. Kimura, PTP 42 (‘69) 1191; 44 (‘70) 1353.
GR related research at RITP
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2nd post-Newtonian formalism for many body systems
T. Ohta, H. Okamura, K. Hiida and T. Kimura,
PTP 50 (‘73) 492; 51 (‘74) 1220; 51 (‘74) 1598.
Gradient expansion for cosmological perturbations
K. Tomita, PTP 54 (’75) 730.
[cf. Salopek and Bond, PRD42 (‘90) 3936.]
Curvature perturbation from inflation
MS, PTP 76 (‘86) 1036.
(2+1) dimensional quantum gravity
A. Hosoya and K. Nakao, PTP 84 (‘90) 739.
GR related research at RITP
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RIFP Kyoto University
Established in 1953 as the first joint-research center for theoretical physics, which is a new type of research center with its facilities open for use for research collaborations by the entire community of theoretical physicists in Japan.
Apparently this was possible thanks to Yukawa’s Nobel Prize.
Yukawa advocated astrophysics and cosmology, but not GR much.
GR became an important area after Humitaka Sato joined RIFP in 1971.
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GR related research at RIFP
Tomimatsu-Sato solution (distorted Kerr)
A. Tomimatsu and H. Sato, PRL 29 (‘72) 1344.
Cosmological/astrophysical constraints on Higgs mass
K. Sato and H. Sato, PTP 54 (‘75) 1564.
Annual workshops on Nuclear Astrophysics (which includes GR and cosmology): ‘55 ~ ‘90
lead by C. Hayashi and later by H. Sato.
GRG workshops: ‘74, ‘75, ’76.
lead by R. Uchiyama, H. Nariai and H. Sato.
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JGRG annual workshops (1991~)
Unification of RITP Hiroshima U and RIFP Kyoto U to form Yukawa Institute for Theoretical Physics was a stimulative event that lead to expansion of the GR community in Japan.
At the same time, various GW detector projects worldwide made research in GR more observationally important.
Also progress in cosmology made GR indispensable for proper understanding of physics of the early universe and its observational consequences.
This year we celebrated 25th anniversary of JGRG workshops
(# of JGRG members ~ 200)
http://www-tap.scphys.kyoto-u.ac.jp/jgrg/index.html
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Gravity Today No deviation from General Relativity
•solar system tests – PPN parameters
:
:
2
00 1 2 2 1
1 2 1
GR
ij ij GR
g
g
|1|<2.3x10-5 : Shapiro time delay (Bertotti et al. ‘03)
|43|<4.4x10-4 : Strong EP (Baessler et al. ‘99)
•constancy of gravitational constant
|dlogG/dt|<10-12 yr-1: Lunar laser ranging (Williams et al ‘04)
e.g., C. Will’s living review
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•binary pulsar – GW emission rate
B1913+16 1.0013±0.0021GR
P
P
Hulse-Taylor binary (B1913+16)
- orbital change due to GW emission
- periastron time shift
perfect match with GR predictions
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GW physics/astronomy Dawn of GW physics/astronomy
• LIGO has started operation • VIRGO will start to operate soon • KAGRA will start to operate by 2017
more accurate, strong field tests of GR
taken from A. Sesana, arXiv:1307.4086
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[JGWC (Japan Gravitational Wave Committee) was founded in 2013]
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another strong evidence for GR
Cosmology Today
CMB spectrum
at T=2.725K
wavelength [mm]
frequency [GHz]
200 sigma
error-bars
COBE/FIRAS
Big-Bang theory has been firmly established
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Strong evidence for inflation
• highly Gaussian fluctuations • almost scale-invariant spectrum
only to be confirmed (by tensor modes?)
Planck 2013
1 2
0
( ) ( )
2 1 (cos ).
4
T
C
T n n
P
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Fundamental(?) Issues
•Dark Matter
Is it really `matter’?
Perhaps yes, because it gravitates.
fermion? boson?
primordial BH?
something else?
Is there a way to generically distinguish them?
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- apparent accelerated expansion of the universe
• Dark Energy
Is the expansion really accelerating?
observational bias? theoretical prejudice?
How can we confirm acceleration?
- modified gravity vs unknown matter field
w<-1 implies modified gravity, etc...
How to distinguish?
large scale structure formation
any other effective discriminators?
Can we falsify GR?
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comments on modified gravity
IR modification UV modification
long distance short distance
GR
? ?
• time is important in spacetime!
• any smooth function f(x) contains infinitely large Fourier modes ...
• amplitude of Riemann? in which frame?
conformal (& disformal) frames?
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•Inflation
How did inflation begin?
What is ‘inflaton’?
what guarantees homogeneity and isotropy?
new guiding principle / working hypothesis?
what determines the end of inflation / reheating?
flatness / open inflation?
non-Gaussianity? tensor-scalar ratio?
frame-independent definition of inflation?
quantum cosmology/gravity?
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What’s next? Which direction?
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my personal recollections cosmological perturbation
theory (CPT)
collaboration with H Kodama
gravitational waves (GW)
collaboration with T Nakamura
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my personal recollections
during 80’s, GWs were regarded as more realistic, of firm GR foundation.
during 90’s, CPT became realistic, thanks to COBE measured anisotropy.
during 00’s, both became realistic. But...
so WE need fairy tales...
fairy tales are necessary for healthy growth of children (H Sato at a theory group workshop in ’90s)
cosmological perturbation theory (CPT)
gravitational waves (GW)
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With a bit of 我田引水 (ga-den-in-sui)
which means ‘self advocacy’, more or less...
String Theory Landscape!
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String theory landscape
There are ~ 10500 vacua in string theory
• vacuum energy rv may be positive or negative
• some of them have rv <<MP4
• typical energy scale ~ MP4
Vr
Bousso & Pochinski (’00), Susskind, Douglas, KKLT (’03), ...
4
PM
4
V PMr
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testing string theory landscape in cosmology?
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Cosmic Landscape various vacua realized in the early universe
distribution determined by various factors probability measure, density of states, quantum equilibrium, ...
quantum transitions between various vacua
http://ineedfire.deviantart.com/art/Psychedelic-Multiverse-104313536
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universe jumps around in the landscape by quantum tunneling
• it can go up to a vacuum with larger rv
• if it tunnels to a vacuum with negative rv ,
it collapses within t ~ MP/|rv|1/2.
• so we may focus on vacua with positive rv: dS vacua
0
rv
Sato, Kodama, MS & Maeda (’81)
de Sitter (dS) space ~ thermal state with T =H/2
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Creation of Open Universe
bubble wall
open universe
dS vacuum
de Sitter (dS) vacuum: O(4,1) Euclidean bubble: O(4) nucleated bubble: O(3,1)
=open universe
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Open Universe in the Landscape Universe inside nucleated bubble = spatially open universe
Observational data indicate 1-W0 = WK,0 ~< 10-2 : almost flat
2
2
2 2
1
3 P
aH
a M a
r
Friedmann eq.
K2 2 2 2
11
3 PM H a H
r W W
negative spatial
curvature
density parameter
(“0” stands for current value)
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what if this is the case? two possibilities
1. inflation after tunneling was short enough (N~60)
W 2 3
01 10 ~ 10
W01 1
2. inflation after tunneling was long enough (N>>60)
signatures from bubble collisions
“open universe”
“flat universe”
signatures in large angle CMB anisotropies?
Kanno, MS & Tanaka (‘13), White, Zhang & MS (’14), …
Sugimura, Yamauchi & MS (‘12)
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0
cos1
T
TA
T
T
l
lCll 1
dipolar statistical anisotropy Kanno, MS & Tanaka (’13)
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isoT
TA
T
T
cos1
Planck XXIII
0.07A
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curvature radius
size of observable universe
Gradient of a field over the horizon scale = Super-curvature mode in open inflation
may modulate the amplitude of
perturbation depending on the direction.
leading order effect is dipolar
if this is the case, then W ~>10-3
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scalar suppression on large scales
scalar
tensor
curvature radius
H0-1 if WK ≈ 0.003
suppression is due to quantum tunneling effect on vacuum
White, Zhang & MS (’14)
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non-Gaussian bubbles in the sky
detection of a spherically symmetric “localized” non-Gaussianity will be the first observational signature of string theory!
3 2
( , ) ( , )NL
T Tf
T T
Sugimura, Yamauchi & MS (’12)
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Summary: future perspectives
precision cosmology
gravitational wave astronomy
We are entering an era of
perturbative, non-perturbative, numerical, observational...
develop “realistic” GR cosmology
any tiny deviation from GR would be revolutionary
look for interesting “fairy tales”
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string landscape, quantum cosmology, something exciting...