emergence of space-time from matrices...distance physics. 4. proof of large-n reduction there are...
TRANSCRIPT
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Emergence of space-time
from
matrices
Feb 25, 2019at IHES
Hikaru Kawai (Kyoto univ.)
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Outline of the talk
Large-N reduction
IIB matrix model
Topology change of space-time
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Large-N reduction
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1. What is Large-N reduction?
Large-N reduction is a typical example of emergence of space-time from matrices.
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The basic statement is
“The large-N gauge theory with periodic
boundary condition does not depend on the
volume of the space-time.”
In particular, the theory in the infinite
space-time is equivalent to that on one point.
The space-time emerges from the internal
degrees of freedom of the reduced model.
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Lattice version
Consider U(N) or SU(N) lattice gauge theory
† †
ˆˆWilson , , , ,
,
n n n n
n
NS Tr U U U U
in a d-dimensional periodic box of size
𝑳𝟏 × 𝑳𝟐 × ⋯× 𝑳𝒅 .
In the large-N limit 𝑵 → ∞, 𝝀: 𝐟𝐢𝐱𝐞𝐝,
physics does not depend on the size of
the box 𝑳𝒊 if the center invariance
𝑼𝒏,𝝁 → 𝒆𝒊𝜽𝝁𝑼𝒏,𝝁
is not broken spontaneously.
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Wilson
1 2
log , exp ,
,d
F Z Z dU S
V L L L
Here “physics” means
(1) Free energy per unit volumeF
fV
(2) Wilson loop
Wilson loop in a periodic box is defined as the next two slides:
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ˆˆ ˆ ˆ, , , , ,
, , 1, 2, , .
C n n n n
d
n
ˆn ˆˆn
ˆn
First of all a closed loop C in the infinite lattice space is specified by a starting point 𝒏 and the sequence of directions 𝜶,𝜷,⋯ .
Therefore we can define the corresponding loop C’ that is folded in the periodic box by the same expression once the starting point n’ is specified:
ˆˆ ˆ ˆ' ', ' , ' , , ' .C n n n n
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Then the Wilson loop in the periodic box is defined as usual:
, Wilson
,
, Wilson
,
ˆ ˆ, , ,
exp
exp
1.
n
n
n
n
n n n
dU S w C
W CdU S
w C Tr U U UN
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Lattice version
Consider U(N) or SU(N) lattice gauge theory
† †
ˆˆWilson , , , ,
,
n n n n
n
NS Tr U U U U
in a d-dimensional periodic box of size
𝑳𝟏 × 𝑳𝟐 × ⋯× 𝑳𝒅 .
In the large-N limit 𝑵 → ∞, 𝝀: 𝐟𝐢𝐱𝐞𝐝,
physics does not depend on the size of
the box 𝑳𝒊 if the center invariance
𝑼𝒏,𝝁 → 𝒆𝒊𝜽𝝁𝑼𝒏,𝝁
is not broken spontaneously.
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if we consider the minimum size of the box 𝟏 × 𝟏 × ⋯× 𝟏,
we have a model with dunitary matrices:
† †
reduced
1
.dN
S Tr U U U U
“the large-N reduced model”
In particular,
1U 2U
3U
1U
2U
†
1U
†
2U
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22
,4
dN
S Tr A A
The large-N reduced model
is equivalent to the d-
dimensional Yang-Mills
if the eigenvalues of 𝑨𝝁
are uniformly distributed.
However, it is not automatically realized.
It is known that the eigenvalues collapse
to one point unless we do something.
Continuum version
𝐴𝜇: 𝑁 × 𝑁
Hermitian
⇔ center invariance
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2. How is the center invariance broken spontaneously?
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To be concrete we consider the continuum
version.
In order to examine the center invariance,
let’s consider the one-loop effective action
for the diagonal elements of 𝑨𝝁 obtained
after integrating out the off-diagonal
elements:(1)
( )N
p
A
p
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The quadratic part of the action
and the one-loop effective action becomes
2(1 loop) 2 ( ) ( )
eff 2 log .i j
i j
S N d p p
2
, .S Tr A A
is given by
2
2
22( ) ( )
,
2 * *( ) ( )
, , , ,
, , ,
,
i j
i ji j
i j
i j j i i j j ii j
S Tr P A P b P c
p p A
p p b c b c
(1)
( )
: off diagonal
0
0 N
A P A
p
P
p
A
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If d > 2, the eigenvalues of 𝑨𝝁 are
attractive, and collapse to a point.
is of order N2 for N variables.
It is minimized in the large-N limit.
(1 loop)
effS
This indicates the spontaneous breaking
of the translational invariance of the
eigenvalues:
This is the continuum version of the
center invariance:
expU iaA A A c
iU e U
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3. How can we recover the center invariance?
In order for space-time to emerge from matrices, the center invariance should be recovered.
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Strong coupling
If the coupling is sufficiently strong,
quantum fluctuation might overwhelm
the attractive force.
It actually happens at least for the lattice
version of the reduced model.
† †
reduced
1
, ~ 4.d
c
NS Tr U U U U
Actually there are several ways to recover
the center invariance.
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quenching
We constrain the diagonal elements of 𝑨𝝁
to a uniform distribution by hand
(𝑨𝝁)𝒊𝒊= 𝒑𝝁(𝒊)
.
Then the perturbation series reproduce
that of the d-dimensional gauge theory.
However, this is rather formal, and the
gauge invariance is no longer manifest.
A lattice version of quenching that keeps
manifest gauge invariance was proposed,
but now it is known that it does not work.Bhanot-Heller-Neuberger, Gross-Kitazawa
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twisting
(0) ˆ
ˆ ˆ, ( ),
A p
p p i B B
the theory is equivalent to gauge theory
in a non-commutative space-time.
If we expand around the non-
commutative back ground
A
Gonzalez-Arroyo, Korthals Altes (‘83)
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Because the equation of motion of the
reduced model is given by
, , 0,A A A
the non-commutative back ground
is a classical solution.
But it is not the absolute minimum of the
action.
One way to make it stable is to modify the
model to
22
, .4
dN
S Tr A A i B
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The lattice version of this is called the
twisted reduced model:
† †
reduced
1
.d
iNS e Tr U U U U
Gonzalez-Arroyo, Okawa
Several MC analyses have been made on the
twisted reduced model, and they found some
discrepancy from the infinite volume theory,
which is related to the UV-IR mixing.
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Heavy adjoint fermions
They have introduced
additional heavy adjoint
fermions.
Kovtun-Unsal-Yaffe (2007),Bringoltz-Sharpe (2009),Poppitz, Myers, Ogilvie, Cossu, D’Elia, Hollowood, Hietanen, Narayanan,Azeyanagi, Hanada, Yacobi
Then the collapse of the eigenvalues can
be avoided without changing the long
distance physics.
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4. Proof of Large-N reduction
There are several proofs, each of which shows an aspect of the large-N reduction.
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Loop equations are nothing but SD equations
obtained from the variation of a link variable
on a Wilson loop.
Loop equations
For example, for a non self intersecting loop
it looks like
1
1
0
the variation
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However for the corresponding folded loop
in a periodic box we have additional terms:
1
1
𝐶1 𝐶2
Here each of 𝐶1 and 𝐶2 is closed in the
periodic box but not in the infinite space.
0
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In the large N limit, traced operators are
factorized in general, and we have
𝒘 𝑪𝟏 𝒘 𝑪𝟐 = 𝒘 𝑪𝟏 𝒘 𝑪𝟐 .
The crucial point is that
𝐶1 (or 𝐶2) contains different numbers of 𝑼𝒏,𝝁
and 𝑼𝒏,𝝁†
at least for one direction μ, because
it is not closed in the infinite space.
Therefore if the center invariance
𝑼𝒏,𝝁 → 𝒆𝒊𝜽𝝁𝑼𝒏,𝝁
is not broken spontaneously, 𝒘 𝑪𝟏 is zero,
and the additional terms disappear.
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Strong coupling expansion
The essence is captured by the Weingarten
model that is obtained from the Wilson
action by replacing the unitary measure with
the Gaussian measure:
“The strong-coupling expansion series of the
Wilson action and the reduced model agree
in the large-N limit.”
Weingarten
† † †
ˆˆ, , , , , ,
, ,
.n n n n n n
n n
S
NTr V V V V N Tr V V
, : complex matrixnV N N
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Wilson loop is simply defined by replacing 𝑼𝒏,𝝁 with 𝑽𝒏,𝝁 :
, Weingarten
,
, Weingarten
,
ˆ ˆ, , ,
exp
exp
1,
n
n
n
n
n n n
dV S w C
W CdV S
w C Tr V V VN
where†
ˆ, , .n nV V
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1
2
3
nC
Then the Feynman diagrams for a Wilson loop look like
Each face corresponds to the 𝑽𝟒 interaction.
Each side corresponds the propagator.
n 1
1
1
1
2 2 2 2
33
3 3
1n
ˆ ˆ1 2n 2n
C
ˆ ˆ1 3n 3n
ˆ ˆ ˆ1 2 3n ˆ ˆ2 3n
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Suppose a vertex A corresponds to the site n .
For any vertex B find a path P from A to B,
B
P
n 1
1
1
1
2 2 2 2
33
3 3
A
The site corresponding to B is obtained by summing up the displacement vectors along P:
ˆ ˆ ˆ3 1 .2n This does not depend on the choice of P,
The crucial point is that we do not need the precise information of the sites if the graph is planar:
The situation is analogous to the existence of apotential for a rotation free vector field.
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This means that Weingarten model and the reduced Weingarten model give the same values of Wilson loop.
A similar analysis can be applied to the
Wilson action by using the standard source
formula:
,
,
Wilson ,
, ,0
Wilson ,
,0
exp , exp
,
exp exp
n
n
n
n nJ
n
nJ
i iS w C f J
N J N J
W C
iS f J
N J
† †exp exp ( .f J dU i N Tr JU Tr J U
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We can show that
the strong-coupling expansion series of the
Wilson action and the reduced model agree
in the large-N limit.
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Perturbative expansion around
diagonal background
2
2 2 31 1 1,
2 2 3
: hermitian matrix,
dS d xTr m
N N
As the simplest example we start with the
large-N 𝝓𝟑 theory in the continuum space,
and the expectation values of single trace
operators such as
1 2 1 2, , , .n n nO x x x Tr x x x
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Parisi’s reduced model
(1) Let be N ×N diagonal
matrices whose elements distribute
uniformly in the d- dimensional space,
which we regard as the momentum
space.
ˆ 1, ,P d
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(2) Corresponding to the field ,
introduce a N ×N Hermitian matrix ,
and construct the corresponding action
and operators by substituting
ˆ ˆexp exp ,x x i P x i P x
x
to the original expression.
21 .
d
dd x
For the action the space-time integral of 1
should be replaced with
Λ is the cut off that appears in . P
Volume of the unit cell
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ˆ ˆexp exp
ˆ ˆ ˆexp , exp ,
x
x i P x i P x
i P x iP i P x
Then we have
2
2 2 3
22 2 3
22 2 3
1 1 1
2 2 3
1 1 1ˆ ,2 2 3
2 1 1 1ˆ , ,2 2 3
d
d
d
S d x Tr m
S d xTr iP m
Tr iP m
← no x
dependence
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“In the large-N limit the expectation value
exp
exp
d O SO
d S
agrees with the original field theory.”
22 2 32 1 1 1ˆ , ,
2 2 3
d
S Tr iP m
action
operators
Thus we obtain
1 2 1 2, , , .n n nO x x x Tr x x x
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For simplicity, we consider the free energy.
The generalization to the expectation values
of the operators are straightforward.
22 2
( ) ( ) 2
,,
ˆ , ,i j
i ji j
Tr P p p m
the propagator for is given by
2
( ) ( ) 2
1.
2
d
i jp p m
j
i
From the quadratic part
,i j
Proof of Parisi’s rule
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Feynman diagrams are something like
ikj
2
2 2 2( ) ( ) 2 ( ) ( ) 2 ( ) ( ) 2
1.
2
d
i j j k k ii j k p p m p p m p p m
In the large-N limit we can replaced
di
Nd p
3
2
2 2 22 2 2
1
2
d
D D D
d
Nd p d p d p
p p m p p m p p m
2 3 1 2
2 2 2 2 2 2
1 2 1 2
1
(2 ) (2 ) (
2
)
d d
d d
dd k d k
Nk m k m k k m
free energy per unit cell end
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We apply Parisi’s rule to the continuum
gauge theory.
,
,
ˆ ˆ ˆ ˆexp , , , exp
ˆ ˆ ˆ ˆexp , exp
iF x i A x i A x
i A x i A x A x A x
i P x P A A P A A i P x
i P x P A P A i P x
ˆ ˆexp expA x i P x A i P x
ˆ ˆ ˆexp , expA x i P x i P A i P x
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22
, ,4
dN
S Tr A A
the action becomes
ˆ ,A P A If we define
and 𝑃𝜇’s disappear from the theory.
One might conclude that this theory is
equivalent to the gauge theory in d-dimensions.
But it is too naïve.
2
2
4
2 ˆ ˆ,4
d
d
NS d xTr F x
NS Tr P A P A
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Actually, in the proof of Parisi’s rule, we
have assumed that the diagonal elements
are negligible, because we have only N
such variables while the action is of order
N2.
But it is not necessarily true in massless
theory.
In that case, the propagators
for diagonal elements become
infinite.
ikj
2 2 2( ) ( ) 2 ( ) ( ) 2 ( ) ( ) 2
1.
i j j k k ii j k p p m p p m p p m
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We have to be careful, when we apply
Parisi’s rule to a massless theory such
as gauge theory.
This is why we have to worry about the
center invariance.
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S becomes the action of gauge theory in a non-
commutative space-time.
Expansion around non-commutative
background
(0) ˆ
ˆ ˆ, ( ),
A p
p p i B B
(0) ˆ .A A a
if we expand 𝑨𝝁 in the matrix model action
21,
4S Tr A A
around a non-commutative back ground
As I said for the twisted reduced model,
This can be shown in the next two slides:
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ˆ ˆ( )exp( ) ( ) ( )exp( )(2 ) (2 )
d d
d d
d k d ko o k ik x o x o k ik x
ˆ ˆ , .x C p B C
Then we have the following correspondence
1 2 1 2
ˆ ˆ, ,
ˆ ˆ * ,
p o i o
o o o o
First we introduce a mapping between
operators and functions
and identity
/ 2
detˆ ( ).
2
d
d
BTr o d x o x
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Then the matrix model action becomes a field
theory on the non-commutative space-time:
2
/ 2*
det B 1
42
d
dS d x F
The crucial point is that the commutator
𝑨𝝁 , 𝑨𝝂 is mapped to the field strength in the
noncommutative space-time:
*
ˆ ˆ ˆ ˆ, ,
ˆ ˆ ˆ ˆ ˆ ˆ ˆ ˆ, , , ,
* *
.
A A p a p a
p p p a a p a a
iB i a i a a a a a
iB i F
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Naively, if UV-IR mixing is not there, this theory is
equivalent to the large-N gauge theory in the low
energy region. But it is not true, and the matrix
theory is not completely equivalent to the ordinary
field theory.
UV-IR mixing and SSB of the center invariance are
related.
† †
reduced
1
diN
S e Tr U U U U
is equivalent to the original reduced model in the
strong coupling region, because the phases cancel out
in the strong coupling expansion.
Actually the twisted reduced model
⇒ no UV-IR mixing in the strong coupling region
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5. Large-N reductionand string theory
Large-N reduced model looks like world sheet string theory.
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The basic idea
For simplicity, we start with bosonic string.
In fact, in the Schild action, the worldsheet
can be regarded as a symplectic manifold,
and the action is given by the integration of
a quantity that is expressed in terms of the
Poisson bracket.
“Worldsheet of string has a structure of
phase space.”
This situation becomes manifest when we
express the string in terms of the Schild
action.
Nambu (‘77)
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Bosonic string is described by the Nambu-Goto
action
2 21, .
2
ab
NG a bS d X X
Schild action
It is nothing but the area of the worldsheet, which is
expressed in terms of an anti-symmetric tensor 𝚺𝝁𝝂
that is constructed from the space-time coordinate
𝑿𝝁.
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It is known that the Nambu-Goto action is
equivalent to the Schild action
2
2 2
Schild
1, ,
2 4 2S d g X X d g
: a volume density on the world shee
1, ,
t
ab
a bX Y
g
X Yg
which is nothing but the Poisson bracket if
we regard the worldsheet as a phase space.
2
Schild
22
Schild
10
2
1.
2 2
ab
a b
ab
a b
S g X Xg
S d X X
The equivalence can be seen easily, by eliminating
𝒈 from the Scild action:
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The crucial point is that the Schild action
has a structure of phase space.
21
, .2 4 2
X X
In fact it is given by the integration over the
phase space
of a quantity that is expressed in terme the
Poisson bracket
2d g
Symplectic structure of the worldsheet
Note that we do not need Worldsheet metric, but
what we need is just the volume density 𝒈.
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Matrix regularization
Then we want to discretize the worldsheet
in order to define the path integral.
2
-symm
function matrix
1, ,
1
etry ( )-symmet y
2
r
A B A Bi
d g A T
W U N
rA
A natural discretization of phase space is
the “quantization”.
If we quantize a phase space, it becomes
the state-vector space, and we have the
following correspondence:
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Then the Schild action becomes
2
Matrix
1, 1 ,
4S Tr A A Tr
and the path integral is regularized like
Schild Matrix
1
exp exp .vol(Diff ) ( )n
dg dX dAZ iS iS
SU n
Here we have used the fact that the phase
space volume is diff. invariant and
becomes the matrix size after the
regularization.
Therefor the path integral over
becomes summation over .
2d g 1Tr n
g
n
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Multi-string states
One good point of the matrix regularization is
that all topologies of the worldsheet are
automatically included in the matrix integral.
Disconnected worldsheets are also included as
block diagonal configurations as
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Furthermore the sum over the size of the
matrix is automatically included, if the
worldsheet is imbedded in a larger matrix
as a submatrix.
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If we take this picture that all the worldsheets
emerge as submatrices of a large matrix, the
second term of
2
Matrix
1, 1
4S Tr A A Tr
can be regarded as describing the chemical
potential for the block size.
Thus we expect that the whole universe is
described by a large matrix that obeys
21, .
4S Tr A A
This is nothing but the large-N reduced model.
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On the other hand, if we start from type IIB
superstring, we will get the reduced model for
supersymmetric gauge theory. In this case
eigenvalues do not collapse, and we can have
non-trivial space-time.
We have seen that in this model the
eigenvalues collapse to one point, and it can
not describe an extended space-time.
This might be related to the instability of
bosonic string by tachyons.
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IIB matrix model
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1. Definition of IIB matrix model
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Schild action of IIB string
First we constract the Schild action of
type IIB superstring.
Green-Schwarz action
2 2
1 1 2 2
1 1 2 2
1 1 2 2
1
2
,
,
GS
ab
a b b
ab
a b
ab
a b
a a a a
S d
i X
X i i
1 2
( 0 ~ 9)
, : 10D Mayorana-Weyl
X
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κ-symmetry
1 1
2 2
1 1 2 2
1 1
2 2
2
1
1 ,
1
12
2
X i i
N=2 SUSY1 1
SUSY
2 2
SUSY
1 1 2 2
SUSY X i i
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Gauge fixing for the κ-symmetry 1 2
2 212 ,
2
.
ab
GS a b
ab
a b
S d i X
X X
N=2 SUSY should be combined with 𝜿 symmetry
so that the gauge condition is maintained1 1 1
SUSY
2 2 2
SUSY
1 2
SUSY
1 21
1 22
2
2
X X X
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N=2 SUSY becomes simple if we consider a
combination
1
2
1
2
2
1
12
2
0.
X i
X
1 2
1 2
2
.2
Then we have the following simple form:
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Schild action
N=2 SUSY
Schild
22 21
, , ,2 4 2 2
S
id g X X X d g
1
1
2
2
1,
2
0
X X
X i
X
Everything is
written in terms of
Poisson bracket.
Then we convert the action to the Schild action
as in the case of bosonic string:
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Matrix regularization
1
1
2
2
1
2
0
F
A i
A
2
Matrix
1 1, , 1 .
4 2S Tr A A A Tr
N=2 SUSY
Applying the matrix regularization, we have
,F i A A
Everything is
written in terms of
commutator.
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IIB matrix model
2
Matrix
1 1, , .
4 2S Tr A A A
Drop the second term, and consider large-N
Formally, this is the large-N reduced
model of 10D super YM theory.
A good point is that the N=2 SUSY is
manifest even after the discretization.
IIB matrix model
Ishibashi, HK, Kitazawa, Tsuchiya
Jevicki, Yoneya
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N=2 SUSY
One of the N=2 SUSY is nothing but the
supersymmety of the 10D super YM theory.
1
1
1
2F
A i
2
Matrix
1 1, ,
4 2S Tr A A A
Even so, they form non trivial N=2 SUSY:
2
20A
The other one is almost trivial.
1 1 2 2 1 2, 0, , 0, , .Q Q Q Q Q Q P
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IIB matrix model is nothing but the
dimensional reduction of the 10D super YM
theory to 0D.
The other matrix modelscomment
It is natural to think about the other possibilities.
In fact, they have considered the dimensional
reduction to various dimensions:
0D ⇒ IIB matrix model
1D ⇒Matrix theory
2D ⇒Matrix string
4D ⇒AdS/CFT
Motl, Dijkgraaf-Verlinde-Verlinde
de Witt-Hoppe-Nicolai,Banks-Fischler-Shenker-Susskind
⇒O’Connor’s
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From the viewpoint of the large-N reduction,
they are equivalent if we quench the diagonal
elements of the matrices.
However the dynamics of the diagonal elements
are rather complicated.
At present the relations among them are not
well-understood.comment end
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Open questions
We expect that the IIB matrix model
)],[2
1],[
4
1(
1 2
2 AAATr
gS
gives a constructive definition of superstring.
However there are some fundamental
open questions:
Is an infrared cutoff necessary?
How should the large-N limit be taken?
How does the space-time emerge?
How does the diff. invariance appear?
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2. Ambiguities in the definition
• Euclidean or Lorentzian• Necessity of the IR cutoff• How to take the (double) scaling limit
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Euclidean or Lorentzian?
In general, systems with gravity do not
allow a simple Wick rotation, because the
kinetic term of the conformal mode (the
size of the universe) has wrong sign.
On the other hand, the path integral of the
IIB matrix model seems well defined for the
Euclidean signature, because the bosonic
part of the action is positive definite:
2
2
1 1[ , ] .
24
1[ , ]S A AA TrTr
g
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How about Lorentzian signature?
If we simply apply the analytic continuation
the path integral becomes unbounded:
0 10 ,A iA
2
0 2 2
2
exp ,
1 1 1[ , ][ , ] [ , ]
4 2
1 1 1[ , ] [ , ] .
2 4
M
M
i i j
Z dAd S
S Tr A A A A Tr Ag
Tr A A A Ag
From the point of view of the large-N
reduction, it is natural to take
exp .MZ dAd i S
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Is IR cutoff necessary?
Because of the supersymmetry
the force between two
eigenvalues cancels between
bosons and fermions
2
(1 ) ( ) ( )
,
2 log 0loop i j
eff F
i j
S D d p p
It seems that we have to impose an infrared
cutoff by hand to prevent the eigenvalues
from running away to infinity.
eigenl A l
(1)
( )N
p
A
p
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But there is a subtlety.
Because the diagonal elements of fermions are
zero modes of the quadratic part of the action,
we should keep them when we consider the
effective Lagrangian.
The one-loop effective Lagrangian for the
diagonal elements is given by
(1)
( )N
p
A
p
1
N
4 8
, ,1-loop
eff
2, 2,
, ,4 8
.
i j i j
i j
i ji j i j
i ji j
S SS x tr
p pS
p p
Aoki, Iso, Kitazawa, Tada, HK
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Because of the fermionic degrees of freedom,
there appears a weak attractive force between
the eigenvalues, and at least the partition
function becomes finite.
However it is not clear whether all the
correlation functions are finite or not.
Austing and Wheater,Krauth, Nicolai and Staudacher,Suyama and Tsuchiya,Ambjorn, Anagnostopoulos, Bietenholz, Hotta and Nishimura,Bialas, Burda, Petersson and Tabaczek,Green and Gutperle,Moore, Nekrasov and Shatashvili.
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1-loop(1 loop) 16 ( )
effexp ,i
i
Z p d S p
( , )i jS i j
( , ) 0, 8n
i jS n
Since is quadratic in ,
which has only 16 components, we have
and
4 8
, ,1-loop
eff
4 8
( , ) ( , )
exp , exp4 8
1 tr tr .
i j i j
i j
i j i j
i j
S SS p tr
a S b S
Let’s estimate the order of this interaction.
We first integrate out the fermionic variables
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4 8
( , ) ( , )1, tr , tri j i ja S b S
16 ( )
1
Ni
i
d
(1 loop)
various terms
exp .
i j i jZ p f p p f p p
O N
Therefore, for each pair of i and j we have 3
choices
which carry the powers of
0, 8, 16 respectively.
Therefore the number of factors other than 1
should be less than or equal to 2N, and we
can conclude that the effective action induced
from the fermionic zero modes is of 𝑶 𝑵 :
.
On the other hand, we have 16N dimensional
fermionic integral .
2N
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.
This should be compared to the bosonic case
2(1 loop)
2
exp 2 log
exp ( )
i j
i j
Z p D p p
O N
SUSY reduces the attractive force by at least
a factor 1/N.
So, in the naïve large-N limit, simultaneously
diagonal backgrounds are stable.
However, it is not clear what happens in the
double scaling limit.
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How to take the large-N limit
In the IIB matrix model , we usually regard
A as the space-time coordinates.
)],[2
1],[
4
1(
1 2
2 AAATr
gS
gSo, has dimensions of length squared.
How is the Planck scale expressed?
If it does not depend on the IR cutoff l, as
we normally guess, we should have1
2Planck .l N g
In other words, we should take the large-N
limit keeping this combination finite.
?
At present we have no definite answer.
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3. Interpretation of the matrices
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What do the matrices stand for?
If we regard the IIB matrix model
)],[2
1],[
4
1(
1 2
2 AAATr
gS
as the matrix regularization of the Schild
action, Aμ are space-time coordinates.
On the other hand if we regard it as the
large-N reduced model, the diagonal
elements of Aμ represent momenta.
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0ˆ 1 , 0, ,3
.0, 4, ,9
kpA
Here satisfy the CCR’sp
Another interesting possibility is to consider a
non-commutative back ground such as
ˆ ˆ, ( ),p p i B B
There are many possibilities to realize the
space-time.
and is the unit matrix.
Then we have a 4D noncommutative flat
space with SU(k) gauge theory.
1k k k
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Actually various models that are close to the
standard model can be constructed by choosing
an appropriate background.
“Intersecting branes and a standard model realization
in matrix models.”
A. Chatzistavrakidis, H. Steinacker, and G. Zoupanos.
JHEP09(2011)115
(ex.)
“An extended standard model and its Higgs geometry
from the matrix model,”
H. Steinacker and J. Zahn,
PTEP 2014 (2014) 8, 083B03
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Expandind universeS.-Kim, J. Nishimura, A. Tsuchiya
Phys.Rev.Lett. 108 (2012) 011601
can be regarded as
an expanding 3+1
D universe.
(ex.)
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Expanding universe 2
Recently another interesting picture of the expanding
universe has been obtained by considering fuzzy
manifolds.
(ex.)
“Quantized open FRW cosmology from Yang-Mills matrix models”
H. Steinacker,
Phys.Lett. B782(2018) 176-180
“The fuzzy 4-hyperboloid 𝑯𝒏𝟒 and higher-spin in Yang-Mills
matrix models”
Marcus Sperling, H. Steinacker,
arXiv:1806.05907
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4. Diffeomorphism invarianceand
Gravity
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Diff. invariance and gravity
Because we have exact N=2 SUSY, it is
natural to expect to have graviton in the
spectrum of particles.
Actually there are some evidences.
(1) Gravitational interaction appears from
one-loop integral.
(2) Emergent gravity by Steinacker. Gravity
is induced on the non-commutative back
ground.
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However, it would be nicer, if we can
understand how the diffeomorphism
invariance is realized in the matrix model.
I would like to introduce an attempt,
although it is not complete.
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Y. Kimura, M. Hanada and HK
The basic question :
In the large-N reduced model, a background
of simultaneously diagonalizable matrices
𝑨𝝁(𝟎)
= 𝑷𝝁 corresponds to the flat space,
if the eigenvalues are uniformly distributed.
In other words, the background 𝑨𝝁(𝟎)
= 𝒊𝝏𝝁
represents the flat space.
How about curved space?
Is it possible to consider some background
like
𝑨𝝁(𝟎)
= 𝒊𝛁𝝁 ?
Covariant derivatives as matrices
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Actually, there is a way to express the covariant
derivatives on any D-dim manifold by D matrices.
More precisely, we consider
𝑴: any D-dimensional manifold,
𝝋𝜶: a regular representation field on 𝑴.
Here the index 𝜶 stands for the components of
the regular representation of the Lorentz group
𝑺𝑶(𝑫 − 𝟏, 𝟏).
The crucial point is that for any representation 𝒓,
its tensor product with the regular representation
is decomposed into the direct sum of the regular
representations:
.r reg reg regV V V V
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In particular the Clebsh-Gordan coefficients for
the decomposition of the tensor product of the
vector and the regular representaion
vector reg reg regV V V V
are written as ,
( ) , ( 1,.., ).b
aC a D
Here 𝒃 and β are the dual of the vector and the
regular representation indices on the LHS.
(𝒂) indicates the 𝒂-th space of the regular
representation on the RHS, and 𝜶 is its index.
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Then for each 𝒂 (𝒂 = 𝟏. . 𝑫),
( )
b
a bC
is a regular representation field on 𝑴.
In other words, if we define 𝛁(𝒂) by
each 𝛁(𝒂) is an endomorphism on the space of the
regular representation field on 𝑴.
Thus we have seen that any covariant
derivative on any D dimensional manifold
can be expressed by D matrices.
,
( ) ( )
b
a a bC
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Therefore any D-dimensional manifold 𝑴with 𝑫 ≤ 𝟏𝟎 can be realized in the space
of the IIB matrix model as
0 ( ) , 1, ,,
0, 1, ,10
a
a
a DA
a D
where 𝛁(𝒂) is the covariant derivative on 𝑴
multiplied by the C-G coefficients.
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Good point 1
Good points and bad points
Einstein equation is obtained at the classical level.
In fact, if we impose the Ansatz ( )a aA i
on the classical EOM , 0,a a bA A A
we have
( ) ( ) ( ), 0
0 , ,
, ( )
0 , 00 .
a a b
a a b
cd cd ca
a ab cd a ab cd ab c
a
d
a b ab b
c
a
R O R O R
R R R
Any Ricci flat space with 𝑫 ≤ 𝟏𝟎 is a
classical solution of the IIB matrix model.
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Good point 2
Both the diffeomorphism and local Lorentz
invariances are manifestly realized as a part of
the 𝑺𝑼(𝑵) symmetry.
In fact, the infinitesimal diffeomorphism and
local Lorentz transformation act on 𝝋𝜶 as
𝝋 → 𝟏 + 𝝃𝝁𝝏𝝁 𝝋 and
𝝋 → 𝟏 + 𝜺𝒂𝒃𝑶𝒂𝒃 𝝋 , respectively.
Both of them are unitary because they preserve
the norm of 𝝋𝜶
𝝋𝜶𝟐 = ∫ 𝒅𝑫𝒙 𝒈 𝝋𝜶∗𝝋𝜶
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Bad points
Fluctuations around the classical solution
𝑨𝒂(𝟎)
= 𝒊𝛁(𝒂)
1. contain infinitely many massless states.
2. Positivity is not guaranteed.
This can be seen by considering the
fluctuations around the flat space.
In this case the background is equivalent to
𝑨𝒂(𝟎)
= 𝒊𝝏𝒂 ⊗ 𝟏𝒓𝒆𝒈 ,
where 𝟏𝒓𝒆𝒈 is the unit matrix on the space of
the regular representation.
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Because the unit matrix 𝟏𝒓𝒆𝒈 is infinite
dimensional, we have infinite degeneracy, and
in particular we have infinitely many massless
states. → bad point 1
In general, the regular representation contains
infinite tower of higher spins, and we have
many negative norm states. It is not clear
whether we have sufficiently many symmetries
to eliminate those negative norm states.
→ bad point 2
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One possible way out is to consider a non-
commutative version.
What we have done is to regard the matrices
as endomorphisms on the space of the regular
representation fields.
It is easy to show that this space is equivalent
to the space of the functions on the frame
bundle of the spin bundle.
If we can construct a non-commutative version
of such bundle, we can reduce the degrees of
freedom significantly without breaking the
diffeomorphism and local Lorentz invariance.
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Topology change of space-time
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1. Low energy effective action ofQuantum gravity/string theory
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A. Tsuchiya, Y. Asano and HK
Low energy effective action of IIB matrix model
We have seen that any D-dim manifold is
contained in the space of D matrices.
Therefore IIB matrix model should contain the
effects of the topology change of space-time.
As was pointed out by Coleman some years
ago, such effects give significant corrections
to the low energy effective action.
It is interesting to consider the low energy
effective action of the IIB matrix model.
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.)()(
,eff
xOxgxdS
SSScSScScS
i
D
i
kji
kji
kjij
ji
iji
i
ii
Actually we can show that if we integrate out the heavy
states in the IIB matrix model, the remaining low
energy effective action is not a local action but has a
special form, which we call the multi-local action:
Here 𝑶𝒊 are local scalar operators such as
𝟏 , 𝑹 , 𝑹𝝁𝝂𝑹𝝁𝝂 , 𝑭𝝁𝝂 𝑭𝝁𝝂, 𝝍𝜸𝝁𝑫𝝁𝝍 ,⋯ .
𝑺𝒊 are parts of the conventional local actions.
The point is that 𝑺𝐞𝐟𝐟 is a function of 𝑺𝒊’s.
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0 .a a aA A
This is essentially the consequence of the well-
known fact that the effective action of a matrix
model contains multi trace operators.
Then we integrate over 𝝓 to obtain the low energy
effective action.
Here we assume that the background 𝑨 𝒂𝟎 contains
only the low energy modes, and 𝝓 contains the rest.
We also assume that this decomposition can be
done in a SU(N) invariant manner.
More precisely, we first decompose the matrices 𝑨𝒂
into the background 𝑨 𝒂𝟎 and the fluctuation 𝝓 :
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Substituting the decomposition into the action of
the IIB matrix model, and dropping the linear
terms in 𝝓, we obtain
20 0 0 0
0
0
2
20
0
1
4
2 , , , 2 , ,
4 , , , fermion
,
.
a b a b a b a b b a
a b a
a
b
b
a b
S Tr
A A
A
A
A
A A
A
In principle, the 0-th order term 20 0
0 ( ) ( )
1,
4a bS Tr A A
can be evaluated with some UV regularization,
which should give a local action.
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The one-loop contribution is obtained by the Gaussian
integral of the quadratic part.
Then the result is given by a double trace operator as
usual:
𝑾 = 𝑲𝒂𝒃𝒄⋯ , 𝒑𝒒𝒓⋯ 𝑻𝒓 𝑨𝒂𝟎𝑨𝒃
𝟎𝑨𝒄𝟎 ⋯ 𝑻𝒓(𝑨𝒑
𝟎𝑨𝒒𝟎𝑨𝒓
𝟎 ⋯)
The crucial assumption here is that both of the
diffeomorphism and the local Lorentz invariance are
realized as a part of the SU(N) symmetry.
Then each trace should give a local action that is
invariant under the diffeomorphisms and the local
Lorentz transformations:
1-loop
eff
1, ( ) ( ).
2
D
i j i j i i
i j
S c S S S d x g x O x
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In the two loop order, from the planar
diagrams we have a cubic form of local
actions2-loop Planar
eff
, ,
1,
6i jk i j k
i j k
S c S S S
while non-planar diagrams give a local
action2-loop NP
eff .i i
i
S c S
z y
x
x
Similar analyses can be applied for higher loops.
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the low energy effective theory of the IIB matrix
model is given by the multi-local action:
.)()(
,eff
xOxgxdS
SSScSScScS
i
D
i
kji
kji
kjij
ji
iji
i
ii
We have seen that
This reminds us of the theory of baby universes
by Coleman.
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Consider Euclidean path integral which involves
the summation over topologies,
Then there should be a wormhole-like configuration in
which a thin tube connects two points on the universe.
Here, the two points may belong to either the same
universe or different universes.
topology
exp .dg S
If we see such configuration from the side of the large
universe(s), it looks like two small punctures.
But the effect of a small puncture is equivalent to an
insertion of a local operator.
Coleman (1989)
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Summing over the number of wormholes, we have
bifurcated wormholes
⇒ cubic terms, quartic terms, …
4 4
,
( ) ( ) ( ) ( ) exp .i j
i j
i j
c d xd d y g x g y O x O yg S
Therefore, a wormhole contributes to the path
integral as
4 4
,
( ) ( ) ( ) ( )exp .i j
i j
i j
c d x d y g x g y O xg yS Od
x
y
4 4
0 ,
4 4
,
1( ) ( ) ( ) ( )
!
exp ( ) ( ) ( ) ( ) .
n
i j
i j
N i j
i j
i j
i j
c d x d y g x g y O x O yn
c d x d y g x g y O x O y
Thus wormholes contribute to the path integral as
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Although there is no precise correspondence, the
loops in the IIB matrix model resemble the
wormholes.
x
x
𝑥
𝑦 ≅
Probably this phenomenon occurs universally.
We may say that if the theory involves gravity
and topology change, its low energy effective
action becomes the multi-local action.
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2. Fine tunings by nature itself
Multi-local action may provide a mechanism of automatic fine tunings and give a solution to the naturalness problem.
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We consider the action given by
eff ,
( ) ( ).
i i i j i j i j k i j k
i i j i j k
D
i i
S c S c S S c S S S
S d x g x O x
Because 𝑺𝐞𝐟𝐟 is a function of 𝑺𝒊’s , we can express
𝐞𝐱𝐩(𝒊𝑺𝐞𝐟𝐟) by a Fourier transform as
1 2 1 2exp , , , , exp ,eff i i
i
iS S S d w i S
where 𝝀𝒊’s are Fourier conjugate variables to 𝑺𝒊’s,
and 𝒘 is a function of 𝝀𝒊’s .
Physics of the multi-local action
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effexp exp .i i
i
dZ d iS Sd w i
The last integral is the ordinary path integral for
the action
𝒊 𝝀𝒊 𝑺𝒊 = ∫ 𝒅𝑫𝒙 𝒈 𝝀𝒊 𝑶𝒊.
Then the path integral for 𝑺𝐞𝐟𝐟 can be written as
Because 𝑶𝒊 are local scalar operators such as
𝟏 , 𝑹 , 𝑹𝝁𝝂𝑹𝝁𝝂 , 𝑭𝝁𝝂 𝑭𝝁𝝂, 𝝍𝜸𝝁𝑫𝝁𝝍 ,⋯ .
𝒊𝝀𝒊 𝑺𝒊 is an ordinary local action and 𝝀𝒊 are
nothing but the coupling constants.
Therefore the system we are considering is very
close to the ordinary field theory, but we have to
integrate over the coupling constants with weight
𝒘(𝝀𝟏, 𝝀𝟐. ⋯ ).
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If has a sharp peak at ,
we can say that the coupling constants are fixed
to .
exp i i
i
d i S
(0)
(0)
However, it is not clear how to define the value
of the path integral
exp i i
i
d i S
in the Lorentzian theory, because we do not know a priori the initial and final states of the universe.
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Instead, we can take a working hypothesis:
Maximum Entropy Principle (MEP):
Coupling constants are tuned so that the entropy of the universe becomes maximum.
Suppose that we pic up a universe randomly from the multiverse. Then the most probable universe is expected to be the one that has the maximum entropy. (T. Okada and HK)
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If the cosmological evolution is completely
understood, we can calculate the total entropy of
the universe, and in principle all of the independent
low-energy couplings are determined by
maximizing it.
For example if we accept the inflation scenario in which
universe pops out from nothing and then inflates, most
of the entropy of the universe is generated at the stage of
reheating just after the inflation stops. Therefore the
potential of the inflaton should be tuned so that inflation
occurs as much as possible.
Furthermore, if we assume that Higgs field plays the
role of inflaton, the above analysis tells that Higgs
potential should become flat at some high energy scale.
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Actually from the recent experimental data, we
see that
(1) the parameters of the SM indeed seem to be
chosen such that Higgs potential becomes
flat around the Planck scale.
(2) We can obtain realistic cosmological model
of Higgs inflation.
Hamada, Oda, Park, HKBezrkov, Shaposhnikov
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If we introduce a non-minimal coupling
a realistic Higgs inflation is possible.
2R
2 2
, .1 /
h h
P
hV
h M
In the Einstein frame the
effective potential becomes
𝜉 can be as small as 10.
Critical Higgs inflation
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• It is natural to expect that space-time emerges
from matrices.
• But there are various possibilities.
• It is also important to understand the time
evolution of universe.
• In particular matrix models may describe the
very beginning of the universe.
• It is important to develop numerical techniques
to solve space-time matrix models.
• Topology change of universe is automatically
included in matrix models, and it may give a
clue to resolve the naturalness problem.
Summary and conclusions