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Yukawa Institute for Theoretical PhysicsKyoto University
Misao Sasaki
Relativity & Gravitation100 yrs after Einstein in Prague
26 June 2012
2
0. Horizon & flatness problem0. Horizon & flatness problem• horizon problem
43 0
3 3 for ( )
Ga P a P
&&
2 2 2 23( )( )( )ds a d d conformal time:
( )dt
da t
conformal time isbounded from below
1if , na t n gravity=attractive
0 0
finite( )
t
t
dta t
2 2 2 23( )( )ds dt a t d
particle horizon
E
3
• solution to the horizon problem4
3 03
( )G
a P a &&
for a sufficient lapse of time in the early universe
0
00 0
( )
t
tt
dta t
or large enough tocover the present
horizon size
NB: horizon problem≠homogeneity & isotropy problem
4
22
8
3 ;
G KH K
a
• flatness problem (= entropy problem)
42
if in the early universe.| |
,K
aa
?
2
0
0
conversely if at an epoch in the early universe,
the universe must have either
or become completely
collapsed (if )
empty ( by noif w.)
| | /
K
K
K
a
alternatively, the problem is the existence of hugeentropy within the curvature radius of the universe
3 3
3 3 3 3 8700 0 0 10
| | | |
aaS T T T H
K K
(# of states = exp[S])
5solution to horizon & flatness solution to horizon & flatness problemsproblems
spatially homogeneous scalar field:
2 21 1
2 2 ( ), ( )V P V & &
2 23 2 0 if ( ) ( )P V V & &
potential dominated2 if ( ) ( )P V V &=
V ~ cosmological const./vacuum energy
2 decreases rapidly.
Kconst
a
inflation
“vacuum energy” converted to radiationafter sufficient lapse of time
solves horizon & flatness problems simultaneously
2 8
3.
GH const
6
11 .. Slow-roll inflation and vacuum Slow-roll inflation and vacuum fluctuationsfluctuations
• single-field slow-roll inflation
V(V())
2
2 2
3 =0
8 1
3 2
( )
( )
H V
a GH V
a
&& &
& &
2 2 2( ) i jijds dt a t dx dx
22
22
332 1
1 22
HH VV
&& &=
&∙∙∙ slow variation of H
inflation!
metric:
field eq.:
Linde ’82, ...
3
( )VH
&
~ Hta e
may be realized for various potentials
7
comoving scale vs Hubble horizon radiuscomoving scale vs Hubble horizon radius
log log aa((tt)=N)=N
log log LL
tt==ttendend
aL
k
k: comoving wavenumber
1L H
inflation
subhorizon
superhorizon
subhorizon
hot bigbang
kH
a
kH
a
kH
a
kH
a
kH
a
8
e-folding number: Ne-folding number: N
log log aa((tt))
log log LL
LL==HH-1 -1 ~ ~ tt
tt==tt(()) tt==ttendend
end
1( )
( ) ~ln ( )t
tN N Hdt z
NN==NN(())
endend
( )exp[ ( )]
( )a t
N t ta t
LL==HH-1-1~ const~ const
redshift# of e-folds from =(t) until the end of inflation
determines comoving scale k
9
• inflaton fluctuation (vacuum fluctuations=Gaussian)2 2 1
2
, ~ ;kiw tk k k
k
kk e w H
aw
v?
rapid expansion renders oscillations frozen at k/a < H(fluctuations become “classical” on superhorizon scales)
22
3
22 / ~
~ ;k kk a H
H k HH
ak
=
Curvature (scalar-type) PerturbationCurvature (scalar-type) Perturbation intuitive (non-rigorous) derivation
• curvature perturbation on comoving slices
c
H
R & ∙∙∙ conserved on superhorizon scale, for purely adiabatic pertns.
evaluated on ‘flat’ slice (vol of 3-metric unperturbed)
10
Curvature perturbation spectrumCurvature perturbation spectrum
• N - formula
( )( )
end endt
t
HN Hdt d
&
( ) ck k
H Ha a
N HN
R&
2 222
2( ) ;kk Hk aH
a
H NP k
R &
2322
22 2k k
k H
~ almost scale-invariant22
2( )
kH
a
HP k
R &• spectrum
MS & Stewart (’96)AA
A
NN
geometrical justification
non-linear extension Lyth, Marik & MS (’04)
Starobinsky (’85)
(rigorous/1st principle derivation by Mukhanov ’85, MS ’86)
11
Tensor PerturbationTensor Perturbation0i TT ij TT
ij ijh h
,
( ; ) ( ) ( ) . .ij k ij kk t a P k t h c
( ):k t same as massless scalar
• canonically normalized tensor field
1 1
232 8;TT TTP
ij ij ij P
Mh h M
G G
: transverse-traceless
2 22 2
2 2 2
4 82 4
2, ,
( )kTT
ij ijP P P
Hh k k
M M M
v v• tensor spectrum
2
4 1
2~ ijS d x g
t
ggg
Starobinsky (’79)
12
Tensor-to-scalar ratioTensor-to-scalar ratio
• scalar spectrum:scalar spectrum: 2
22
2s
HP k N
• tensor spectrum:tensor spectrum: 8
2
2
2 2( )g
P
HP k
M
• tensor spectral index:tensor spectral index:2
2 2
2 2 2 22g
P P
Hn
H M H M N
& &&
&
aa
dNH N
dt
g
8gg
s
Pr n
P ··· ··· valid for all slow-roll modelsvalid for all slow-roll models
with canonical kinetic termwith canonical kinetic term
1snk
gnk
1
822
g
sP
P
PM N
2( )ab
a b
N NN G
13
Comparison with observationComparison with observationStandard (single-field, slowroll) inflation predicts Standard (single-field, slowroll) inflation predicts scale-invariant scale-invariant GaussianGaussian curvature perturbations. curvature perturbations.
CMB (WMAP) is consistent with the prediction.
Linear perturbation theory seems to be valid.
WMAP 7yr
14
CMB constraints on inflationCMB constraints on inflationKomatsu et al. ‘10
scalar spectral index: ns = 0.95 ~ 0.98
tensor-to-scalar ratio: r < 0.15
15
However,….
Inflation may be non-standard
multi-field, non-slowroll, DBI, extra-dim’s, …
Quantifying NL/NG effects is important
2gauss gauss
3
55? C ~;NL NLff R R R L
PLANCK, … may detect non-Gaussianity
B-mode (tensor) may or may not be detected.
energy scale of inflation -10 2Planck10 ?2H M
modified (quantum) gravity? NG signature?
(comoving) curvature perturbation:
16
2. Origin of non-Gaussianity2. Origin of non-Gaussianity
• self-interactions of inflaton/non-trivial “vacuum”
• nonlinearity in gravity
• multi-field
classical physics, nonlinear coupling to gravity superhorizon scale during and after inflation
quantum physics, subhorizon scale during inflation
classical general relativistic effect, subhorizon scale after inflation
17
Origin of NG and cosmic scalesOrigin of NG and cosmic scales
log log aa((tt))
log log LL
tt==ttendend
aL
k
k: comoving wavenumber
1L H
inflation
classical gravity
classical/localeffect
quantum effect
hot bigbang
18
OriginOrigin 1:1: self-interaction/non-trivial vacuumself-interaction/non-trivial vacuum
• conventional self-interaction by potential is ineffective
4 V
• need unconventional self-interaction → non-canonical kinetic term can generate large NG
Non-Gaussianity generated on subhorizon scales
(quantum field theoretical)
ex. chaotic inflation2 21
2
V m ∙∙∙ free field!
(grav. interaction is Planck-suppressed)
Maldacena (’03)
21~ ( / )PlO M1510~
extremely small!
19
1a. Non-canonical kinetic term: DBI inflation1a. Non-canonical kinetic term: DBI inflation
1 21~ ( ) ( )K ff &kinetic term:
Silverstein & Tong (2004)
1 1f
~ (Lorenz factor)-1
perturbation expansion
0 1 2 3K K K K K
0
= ∝ ∝
3 3+2
2 20 0~
large NG for large
3 21
2 ;X X f
&
20
Bi-spectrum (3pt function) in DBI inflationBi-spectrum (3pt function) in DBI inflation
fNLlarge for equilateral configuration
1 2 3~ ~p p pv v v
1 2 3 0p p p v v v
2pv
3pv
1pv
1 3
1 21
2
2 3
( ) ( ) ( )
~ ( ) ( ), (( ), )
C C
L
C
j C Cj
N
p p
f p p p
p
p p p R R R
R R cyclic
2~NLf
equil NL NLff
WMAP 7yr: 241 266 95equil CL( % )NLf
Alishahiha et al. (’04)
21
1b. Non-trivial vacuum1b. Non-trivial vacuum
• de Sitter spacetime = maximally symmetric(same degrees of sym as Poincare (Minkowski) sym)
gravitational interaction (G-int) is negligible in vacuum
• slow-roll inflation : dS symmetry is slightly brokenG-int induces NG but suppressed by
(except for graviton/tensor-mode loops)
2/ PlH M &
But large NG is possible if the initial state (or state athorizon crossing) does NOT respect dS symmetry
(eg, initial state ≠ Bunch-Davies vacuum)various types of NG :
scale-dependent, oscillating, featured, folded ...Chen et al. (’08), Flauger et al. (’10), ...
3 1( , )SO
23
Origin 2Origin 2:: superhorizon generationsuperhorizon generation
• NG may appear if T depends nonlinearly on , even if itself is Gaussian.
This effect is small in single-field slow-roll model(⇔ linear approximation is valid to high accuracy)
• For multi-field models, contribution to T from each field can be highly nonlinear.
NG is always of local type:
1 2 3local const.( , , )NL NLf p p p f
Salopek & Bond (’90)
N formalism for this type of NG
x
tot
=A tot
WMAP 7yr: 10 74 95local CL( % )NLf
24
Origin 3Origin 3:: nonlinearity in gravitynonlinearity in gravity
ex. post-Newtonian metric in asymptotically flat space
2 2 2 2 21 2 2 1 2 2ds dt dr
NL (post-Newton) termsNewtonpotential
• important when scales have re-entered Hubble horizon
5~ ( )NLf O
• effect on CMB bispectrum may not be negligible
Pitrou et al. (2010)
(for both squeezed and equilateral types)
(in both local and nonlocal forms)
distinguishable from NL matter dynamics?
?
25
3. 3. N formalismN formalism
• N is the perturbation in # of e-folds counted backward in time from a fixed final time tf
• N is equal to conserved NL comoving curvature perturbation on superhorizon scales at t>tf
• tf should be chosen such that the evolution of the universe has become unique by that time.
• N is valid independent of gravity theory
What is What is N?N?
therefore it is nonlocal in time by definition
=adiabatic limit
26
3 types of 3 types of NN
originally adiabatic
end of/afterinflation
entropy/isocurvature → adiabatic
ft t
1
2
27
NonlinearNonlinear N - formulaN - formulaChoose flat slice at t = t1 [ F (t1) ] andcomoving (=uniform density) at t = t2 [ C
(t1) ] :( ‘flat’ slice: (t) on which )
F (t1) : flat
C(t2) : comoving (t2)=const.
(t1)=0
F(t2) : flat
0 2 12 11 2, , , ; iFN t N t t N t t xt
C2 21, ,; i iF t t x t xN R
(t2)=0
(3) 3 3 ( , ) 3det ( ) ( )t xa t e a t R
28
• Nonlinear N for multi-component inflation :
1 2
1 2
1
!
n
n
A A A
nAA A
AA An
N N N
N
n
where =F is fluctuation on initial flat slice at or after horizon-crossing.
F may contain non-Gaussianity from subhorizon (quantum) interactions
eg, in DBI inflation
2944.. NG generation on superhorizon NG generation on superhorizon scalesscales
• curvaton-type Lyth & Wands (’01), Moroi & Takahashi (‘01),...
two efficient mechanisms to convertisocurvature to curvature perturbations:
curv() << tot during inflation
highly nonlinear dep of curv on possible
curv() can dominate after inflation
curvature perturbation can be highly NG
curvaton-type & multi-brid type
30
• multi-brid inflationMS (’08), Naruko & MS (’08),...
sudden change/transition in the trajectory
21
2a a b
a abN N N L
tensor-scalar ratio r may be large in multi-brid models,while it is always small in curvaton-type if NG is large.
curvature of this surface determines sign of fNL
31
5. Summary5. Summary
• inflation explains observed structure of the universe
flatness: 0=1 to good accuracy
curvature perturbation spectrum
almost scale-invariantalmost Gaussian
• inflation also predicts scale-invariant tensor spectrum
will be detected soon if tensor-scalar ratio r>0.1
any new/additional features?
32
• 3 origins of NG in curvature perturbation
• multi-field model: origin 2.
• DBI-type model: origin 1.
1. subhorizon ∙∙∙ quantum origin
2. superhorizon ∙∙∙ classical (local) origin
3. NL gravity ∙∙∙ late time classical dynamics
equilNLf may be large
localNLf may be large: In curvaton-type models r≪1.
Multi-brid model may give r~0.1.
NG frominflation
need to be quantified
• non BD vacuum: origin 1.
NLfany type of may be large
non-Gaussianitiesnon-Gaussianities