Anisotropic Infaltion
--- Impact of gauge fields on inflation ---
Jiro SodaKyoto University
ExDiP 2012, Hokkaido, 11 August, 2012
2
Standard isotropic inflation
24 4 1 ( )
2 2pM
S d x gR d x g V
222
1 (3 2
)1
p
H VM
3 '( ) 0H V
2 2 2 2 2 2( )ds dt a t dx dy dz
aHa
Isotropic homogeneous universe
Friedman eq.
1/ 2 188 2.4 10 GeVpM G
Action
K-G eq.
a ∝ eHtinflation
3
Origin of fluctuations2
2cHR N H t H
pl
HhM
Curvature perturbations
Tensor perturbations
/ 2plM h The relation yields
The tensor to the scalar ratio2
2
816t
s p
P drP M dN
e
24
8p ij ij
ij ij
MS d x h h h h Action for GW
4 2
2 2 2
14 8s
p
H HPM e
2
2 2
2t
p
HPM
1( )N x 2( )N x
1( )x 2( )x
1( )cR x
一定
2( )cR x
initial
inflation end 1e
2 polarizations
scale invariant spectrum
4
From COBE to WMAP!
,m mm
T a YT
' ' ' 'm m mma a C
CMB angular power spectrum
COBE
TT
: ζgravitational red shift
The predictions have been proved by cosmological observations.
We now need to look at a percent level fine structure of primordial fluctuations!
WMAP provided more precise data!
E and B Polarizations
Primordial gravitational waves via B-modes
Primordial gravitational waves
6
2
0( ) ( ) 1 ( )P k P k g k k n
n : prefered direction
Groeneboomn & Eriksen (2008)
The preferred direction may be produced by gauge fields.
Eriksen et al. 2004Hansen et al. 2009
Statistical Anisotropy?
7
quantitative improvement -> spectral tilt
qualitative improvement -> non-Gaussianity PGW
There are two directions in studying fine structures of fluctuations!
Yet other possibility is the statistical anisotropy
What should we look at?
If there exists coherent gauge fields during inflation, the expansion of the universe must be anisotropic.Thus, we may have statistical anisotropy in the primordial fluctuations.
Gauge fields and cosmic no-hair
8
The anomaly suggests gauge fields?
9
S −
14
4x −g gαgνβFνFαβ
ds2 −t2 α2t x2 y2 z2⎡⎣ ⎤⎦
α2η −η2 x2 y2 z2⎡⎣ ⎤⎦
S −
14
4xα4η1
α2η1
α2ηηαηνβFνFαβ
⎡⎣⎢
⎤⎦⎥
gauge fields
FLRW universe
In terms of a conformal time, we can explicitly see the conformal invariance
cancelled out
Thus, gauge fields are decoupled from the cosmic expansion and hence no interesting effect can be expected.In particular, gauge fields are never generated during inflation.
However, …..
The key feature of gauge fields is the conformal invariance.
Gauge fields in supergravity
10
S 4x −g R gi ∂
i∂−eκ
2Kgi D iW D W −3κ 2 W 2
⎡⎣⎢
⎤⎦⎥
While, the role of gauge kinetic function in inflation has been overlooked.
Cosmological roles of Kahler potential and super potential in inflation has been well discussed so far.
Supergravity action
The non-trivial gauge coupling breaks the conformal invariance because the scalar field has no conformal invariance.
K( : Kahler potential W ( : superpotential fab( : gauge kinetic function
Thus, there is a chance for gauge fields to make inflation anisotropic.
4x −g −
14Re αβ
iFανFνβ −
18I αβ
ie νλρFναFλρ
β⎡⎣⎢
⎤⎦⎥
Why, no one investigated this possibility?
Black hole no-hair theorem
11
MJ
Q
Black hole has no hair other than M,J,Q
gravitational collapse
Israel 1967,Carter 1970, Hawking 1972
any initial configurations
event horizon
By analogy, we also expect the no-hair theorem for cosmological event horizons.
Let me start with analogy between black holes and cosmology.
Cosmic no-hair conjecture
12
Tν ΛΛ
deSitter
Tν
Λ
Gibbons & Hawking 1977, Hawking & Moss 1982
cosmic expansion
Inhomogeneous and anisotropic universe
no-hair ?
Cosmic No-hair Theorem
Dominant energy condition: Strong energy condition:
Assumption:
Statement:
The universe of Bianchi Type I ~ VIII will be isotropized and evolves toward de Sitter space-time, provided there is a positive cosmological constant .
Wald (1983)
0ρ
3 0pρ
, pρ: energy density & pressure other than cosmological constantpρ
0pρ
ex)ex)
a positive cosmological constant
Type IX needs a caveat.
Sketch of the proof
14
21 03
K Kt
Λ
33
tanh 3
Kt
ΛΛ
Λ
Ricci tensor (0,0)
Einstein equation (0,0)
(3)
0R Bianchi Type I ~ VIII :
0 Strong Energy Condition
0 Dominant Energy Condition
−∂K∂t
−13K2 Λ Σ i
Σi
1M
2Tν −
12gνT
⎛⎝⎜
⎞⎠⎟t
tν
3K Λ3t Λin time scale :
213
K Λ
1M
2Tνt
tν(3)1
2R1
2i j
j iΣ Σ
2 2 ( )ijds dt h x dx dx ν 0 1 1
2 3ij ij ij ij ijh K Kt
Σ
0ijΣ 3t Λ
in time scale :
No Shear = Isotropized(3)
0R
00 0T
Spatially FlatNo matter
The cosmic no-hair conjecture kills gauge fields!
15
No gauge fields!Tν
Inflationary universe
Tν
Any preexistent gauge fields will disappear during inflation.Actually, inflation erases any initial memory other than quantum vacuum fluctuations.
Predictability is high!
Since the potential energy of a scalar field can mimic a cosmological constant, we can expect the cosmic no-hair can be applicable to inflating universe.
Initial gauge fields
Can we evade the cosmic no-hair conjecture?
All of these models breaking the energy conditionhave ghost instabilities.
・ Vector inflation with vector potential Ford (1989)
・ Lorentz violation Ackerman et al. (2007)
・ A nonminimal coupling of vector to scalar curvatureGolovnev et al. (2008), Kanno et al. (2008)
Himmetoglu et al. (2009)
1 ( )4
F F V A Aν ν L
21 ( )4
F F A A mν ν λ L
・・・ Fine tuning of the potential is necessary.
・・・ Vector field is spacelike but is necessary.0 0A
2 1 1 14 2 6
i i i iF F m R A Aν ν
L
・・・ More than 3 vectors or inflaton is required
One may expect that violation of energy conditions makes inflation anisotropic.
F A Aν ν ν
Anisotropic inflation
17
Gauge fields in inflationary background
18
S −
14
4x −g 2α FνFν
ds2 −t2 α2t x2 y2 z2
de Sitter backgrounda(ηeHt 1
−Hη α2η −t2 x2 y2 z2⎡⎣ ⎤⎦
abelian gauge fields
It is possible to take the gauge
F A Aν ν ν
gauge symmetry A A ∂ χ
A0 0 , ∂iAi 0
S 12
4x −g 2 ∂Ai
∂η⎛⎝⎜
⎞⎠⎟2
Ai ∂i2 Ai
⎡
⎣⎢⎢
⎤
⎦⎥⎥
Ai 3κ2
3/2σ∑ Aκ
σ ηe iσ κeiκ⋅x
ki e iσ κ0, e i
σ −κe iσ 'κσσ '
12
4x −g 2 ∂Aκσ η∂η
∂A−κσ η∂η
−κ2Aκσ ηA−κ
σ η⎡⎣⎢
⎤⎦⎥
kσ = δ S
δ ∂Akσ / ∂η( )
= f 2A−kσ
f depends on time.
Akσ , κ'
σ '⎡⎣ ⎤⎦iσσ ' κ −κ'canonical commutation relation
f (t
Do gauge fields survive?
19
0 Ai (x)Ai (0) 0 κκ PAκe
iκ⋅x PA (k) κ3 uκη
2
2α2η
Thus, it is easy to obtain power spectrums
P(k)
k
blue
red
The blue spectrum means no gauge fields remain during inflation.
The red spectrum means gauge fields survive during inflation.
Akσ uκηακ
σ uκ*ηα−κ
σ † A−κσ † ∂2 uk
∂η 2 + 21f
∂ f∂η
∂uk
∂η+ k 2uk = 0
Canonical commutation relation leads to commutation relations and the normalization
uk∂uκ
*
∂η−uκ
* ∂uκ
∂η
i2ak
σ , ακ'σ '†⎡⎣ ⎤⎦σσ ' κ−κ'
akσ 0 0vacuum
Mode functions on super-horizon scales
20
sub-horizon
vk uκ∂2 vk
∂η 2 + k2 − 1f
∂2 f∂η 2
⎡⎣⎢
⎤⎦⎥vk = 0
−kη → ∞ vk 12κ
e−iκη uk 1
2κe−iκη
−kη → 0 ∂2 uk
∂η 2 + 2 1f
∂ f∂η
∂uk
∂η= 0 ∂
∂ηf 2 ∂uk
∂η⎛⎝⎜
⎞⎠⎟
= 0 uk χ1 %χ2
η2super-horizon
f αα
⎛⎝⎜
⎞⎠⎟−2χ
da 1−Hη
⎛⎝⎜
⎞⎠⎟
ηHη2 Hα2η
uk χ1 %χ2
αHα2 2
χ1 χ2α4χ−1
ak H κmatching at the horizon crossing
i) c >14
ii) c <14
1fk 2k
χ2ακ4χ−1
1fk 2k
χ1
Take a parametrization
Since we know we get
Length
time
1H
Sub-horizon
Super-horizon
ak
Gauge fields survive!
21
i) c >14
PA (k) κ3 uκη
2
2α2η
H2
Hα
κ⎛⎝⎜
⎞⎠⎟2χ−2
ii) c < 14
PA (k) κ3 uκη
2
2α2η
H2
Hα
κ⎛⎝⎜
⎞⎠⎟−2χ−1
c >1 red spectrum
c <−12
red spectrum
For a large parameter region, we have a red spectrum, which means that there exists coherent long wavelength gauge fields!
Finally, at the end of inflation, we obtain the power spectrum of gauge fields on super-horizon scales
uk 1
κ 2κα
ακ
⎛⎝⎜
⎞⎠⎟4χ−1
uk 1
κ 2κ
We should overcome prejudice!
22
According to the cosmic no-hair conjecture, the inflation should be isotropic and no gauge fields survive during inflation.
However, we have shown that gauge fields can survive during inflation.
It implies that the cosmic no-hair conjecture does not necessarily hold in inflation.
Hence, there may exist anisotropic inflation.
23
S 4x −g
M2
2R −
12
∂ 2−V
⎡
⎣⎢⎢
⎤
⎦⎥⎥ 0
pMV V eλ
22 2 4/ 2 2 2ds dt t dx dy dzλ
In this case, it is well known that there exists an isotropic power law inflation
Gauge fields and backreaction
S 4x −g
M2
2R −
12
∂ 2−V −
142 FνF
ν⎡
⎣⎢⎢
⎤
⎦⎥⎥
0pMf f e
ρ
In this background, one can consider generation of gauge fields
gauge kinetic function
power-law inflation
our universe
H −1
There appear coherent gauge fields in each Hubble volume.Thus, we need to consider backreaction of gauge fields.
M p
= − 2λ
log t
Exact Anisotropic inflation
24
2 28 12 8
6 2λ ρλ ρ
λ λ ρ
2 2 43 2λ ρλzλ λ ρ
2 2 4 0λ ρλ >
ds2 −t2 t2 t−4zx2 t2z y2 z2 ⎡⎣ ⎤⎦
For the parameter region , we found the following new solution
Kanno, Watanabe, Soda, JCAP, 2010
For homogeneous background, the time component can be eliminated by gauge transformation.Let the direction of the vector to be x – axis.
ds2 −t2 e2α t e−4σ tx2 e2σ t y2 z2 ⎡⎣ ⎤⎦
Then, the metric should be Bianchi Type-I
Watanabe, Kanno, Soda, PRL, 2009
ΣH
&σ&α13IeH
2
2
2 42
I λ ρλλ ρλ
eH −&H
H 2
6λ λ 2ρ λ2 8ρλ 12ρ2 8
0 1I <
Apparently, the expansion is anisotropic and its degree of anisotropy is given by
slow roll parameter
A 0, Axt, 0, 0
M p
= −2λ
log t &Ax (t)Ctg g 4 ρλ
−ω − 4ζ
The phase space structure
25
Isotropic inflation
Anisotropic inflation
2 2 4 0λ ρλ >
After a transient isotropic inflationary phase, the universe enter into an anisotropic inflationary phase.
Kanno, Watanabe, Soda, JCAP, 2010
The result universally holds for other set of potential and gauge kinetic functions.
Quantum fluctuations generate seeds of coherent vector fields.
anisotropy
scalar
vector
More general cases
&α 2 &σ 2
13
12&2 V
E2
2−2e−4α−4σ⎡
⎣⎢
⎤⎦⎥
&&α −3&α 2 V
E2
6−2e−4α−4σ
&&σ −3&α &σ
E2
3−2e−4α−4σ
2 3 4 43 ( ) ( ) ( )V E f f e α σ α
Hamiltonian Constraint
Scale factor
Anisotropy
Scalar field
t
'
2 2 2 ( ) 4 ( ) 2 2 ( ) 2 2t t tds dt e e dx e dy dzα σ σ
const. of integration
2 4 ( ) Ev f e α σ
A 0, vt, 0 , 0
( )t
M p 1
&α 2
13
V ⎡⎣ ⎤⎦2
2 4 4( )2
E f e α σ
f e 2 2
Behavior of the vector is determined by the coupling
f (e−2α e2
VV
f e2 2
dα
&α&−
V V
Conventional slow-roll equations(The 1st Inflationary Phase)
3 ( )Vα
Hamiltonian Constraint
Scalar field
212 2σ
2 3 4 4( ) ( )E f f e α σ
c
To go beyond the critical case, we generalize the function by introducing a parameter
c1> Vector grows1 Vector remains const.1< Vector is negligible
α −
VV
Now we can determine the functional form of f2
2
2mV 2( )f e α
Critical Case
The vector field should grow in the 1st inflationary phase.
Can we expect that the vector field would keep growing forever?
E2
2e−χ2 −4α
&α 2
13
⎡⎣ ⎤⎦2
2
2m
χE2 e−χ
2 −4α
Attractor mechanism
R ≡
ρA
ρ
E2e−χ
2 −4α
22
2 3 mα
Hamiltonian Constraint
Scalar field
4σ
4σ
2σ
Define the ratio of the energy density
R ≈
1χ2 ≈O10Typically, inflation takes place at 210
cE2e−χ2 −4α ≈ 2
e−2α e2 2
4( 1)ce α
The opposite force to the mass term
Irrespective of initial conditions, we have 210R=
1c >
12
&2
The growth should be saturated around
Inflaton dynamics in the attractor phase
&α 2
16 22
3 &α &− 2 χE2e−χκ22 −4α
α
−2 2χE2
2e−χ
2 −4α
e−χ2 −4α
2χ−1χ2E2
Hamiltonian Constraint
Scalar field
α
const. of integration
4( 1)cDe α 11
We find becomes constant during the second inflationary phase.Aρ
The modified slow-roll equations: The second inflationary phase
1c
2
3 mc
α E.O.M. for Φ : (2nd inflationary phase)
23 mα (1st inflationary phase)
1c >Remember
ρA
E2
2e−χ
2 −4α
Energy Density
Solvable
m2(c −12χ2
Phase flow: Inflaton
23 m
cα
23 mα
2c Numerically solution at
Scalar field
12
(2nd inflationary phase)(1st inflationary phase)
c0 17 m 10−5
ΣH
≡&σ&αE2e−χ
2 −4α
9 &α 2
The degree of Anisotropy
3 &α &σ
E2
3e−χ
2 −4α
ΣH
23R t
23χ−1χ22
2
αeα
1 13
cH c
eΣ
σ
Anisotropy4σ
2 ( )3
t R
The degree of anisotropy is determined by
The slow-roll parameter is given by
Attractor point
e
2χ2
We find that the degree of anisotropy is written by the slow-roll parameter.
Attractor point
e−χ2 −4α
2χ−1χ2E2
Attractor Point
3 &α 2
12 22:Hamiltonian Constraint
R ≡
ρA
ρ
E2e−χ
2 −4α
22
Ratio
Compare
: A universal relation
Evolutions of the degree of anisotropy
32
c0 17
( ) AtH
ρρ
Σ =R
Numerically solution at
Initially negligible
grows fast
becomes constant disappears
0.3%HΣ
increase
x
Anisotropic Inflation is an attractor
33
ds2 −t2 e2Ht e−4Σ tx2 e2Σ t y2 z2 ⎡⎣ ⎤⎦
13 HI
HeΣ
0 1I <
Statistical Symmetry Breaking in the CMB
It is true that exponential expansion erases any initial memory.In this sense, we have still the predictability. However, the gauge kinetic function generates a slight anisotropy in spacetime.
34
Phenomenology of anisotropic inflation
What can we expect for CMB observables?
35
ρe ∝ IeH
f≈VV
≈1
eH
vector-tensor
vector-scalar
ρe ≈ IeH
f
ρe ≈1
eH
IeH ≈ I
−ggαgνβ 2Fν
ρe ν
1 24 34Fαβ
−ggαgνβ 2
{ Fν
1
2ρe ν
{Fαβ
In the isotropic inflation, scalar, vector, tensor perturbations are decoupled.
z κ1z κ 2 κ1 κ 2Pσκ1 |κ1 |
h(k1)h(k 2 ) κ1 κ 2Ptκ1 |κ1 |
The power spectrum is isotropic
However, in anisotropic inflation, we have the following couplingslength
t
1H
ak
N(k)
Preferred direction
n ∝A
36
Predictions of anisotropic inflation
statistical anisotropy in curvature perturbations
cross correlation between curvature perturbations and primordial GWs
statistical anisotropy in primordial GWs
TB correlation in CMB
224 ( )sg I N k
26 ( )t Hg I N ke
224 ( )c H
Gr I N k
ze
zz
Ps(k) Pσκ 1−gσ ν⋅κ̂
2⎡⎣⎢
⎤⎦⎥
Pt (k) Ptκ 1−gt ν⋅κ̂
2⎡⎣⎢
⎤⎦⎥
Thus, we found the following nature of primodordial fluctuations in anisotropic inflation.
These results give consistency relations between observables.
64gt ρgσ 4c tr g
Watanabe, Kanno, Soda, PTP, 2010Dulaney, Gresham, PRD, 2010Gumrukcuoglu,, Himmetoglu., Peloso PRD, 2010
k̂
preferred direction
n
37
WMAP constraint Pullen & Kamionkowski 2007
Now, suppose we detected
Then we could expect
0.02He
• statistical anisotropy in GWs
• cross correlation between curvature perturbations and GWs
224 ( ) 0.3sg I N k
224 ( ) 0.3sg I N k
31.5 10tg 36 10
Gzzz
If these predictions are proved, it must be an evidence of anisotropic inflation!
How to test the anisotropic inflation?
The current observational constraint is given by
How does the anisotropy appear in the CMB spectrum?
38
* ˆ ˆXYk XY s m s mC d P Y Y W k k k
P P kk XYC
The off-diagonal part of the angular power spectrum tells us if the gauge kinetic function plays a role in inflation.
For isotropic spectrum, , we have
Angular power spectrum of X and Y reads
For anisotropic spectrum, there are off-diagonal components.
For example, *
2ˆ ˆTB
k TB m mC d P Y Y W k k k
, 1
We should look for the following signals in PLANCK data!
39
0.3r 0.3sg
When we assume the tensor to the scalar ratio
and scalar anisotropy
The off-diagonal spectrum becomes
The anisotropic inflation can be tested through the CMB observation!
Watanabe, Kanno, Soda, MNRAS Letters, 2011
Non-gaussianity in isotropic inflation
S 4x −g
12R −
12
∂ 2−V −
142 FνF
ν⎡⎣⎢
⎤⎦⎥
f (eχ22
e−2χα αη−2χ
PA(k)κ3 uκη
2
2α2η
H2
Hα
κ⎛⎝⎜
⎞⎠⎟2χ−2
For c=1, we have the scale invariant spectrum.
a(η1
−HηdeSitter
Pz P 1192 PNCMB2 Ntot −NCMB⎡⎣ ⎤⎦ : P
fNL
local 1280PNCMB3 Ntot −NCMB : 10
−2Ntot −NCMB< 600 Barnaby, Namba, Peloso 2012
k13k3
3 z κ1z κ2
z κ3∝1χoσ2κ̂1⋅κ̂3∝ χoσY0
0 σiνY20 ; 0.22
anisotropy
Non-gaussianity in anisotropic inflation
&α 2
16 22
3 &α &− 2χE2e−χ2−4α
dα
−2
2χ 2
E2e−χ2−4α ec2
χ2E2
2χ−1e−4α
f (eχ22
e−2α αη−2
c >1
ceff 1Scale invariant Is an attractor!
Summary
42
We have shown that anisotropic inflation with a gauge kinetic function induces the statistical symmetry breaking in the CMB.
Off-diagonal angular power spectrum can be used to prove or disprove our scenario.
More precisely, we have given the predictions:
We have already given a first cosmological constraint on gauge kinetic functions.
the statistical anisotropy in scalar and tensor fluctuations the cross correlation between scalar and tensor the sizable non-gaussianity
gs 24 I N2κ < 0.3 I
λ2 2ρλ −4λ2 2ρλ
<0.3
24 N 2κ
Anisotropic inflation can be realized in the context of supergravity.
As a by-product, we found a counter example to the cosmic no-hair conjecture.