expanding (3+1)-dimensional universe from the iib matrix model
DESCRIPTION
Expanding (3+1)-Dimensional universe from the IIB matrix model. Asato Tsuchiya (Shizuoka Univ.) SQS ’2013 @Bogoliubov Laboratory, July 29 th , 2013 . References. Sang-Woo Kim, Jun Nishimura and A. T. PRL 108 (2012) 011601, arXiv:1108.1540 - PowerPoint PPT PresentationTRANSCRIPT
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EXPANDING (3+1)-DIMENSIONAL UNIVERSE FROM THE IIB MATRIX MODEL
Asato Tsuchiya (Shizuoka Univ.)
SQS ’2013 @Bogoliubov Laboratory, July 29th, 2013
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References
Sang-Woo Kim, Jun Nishimura and A. T. PRL 108 (2012) 011601, arXiv:1108.1540 PRD 86 (2012) 027901, arXiv:1110.4803 JHEP 10 (2012) 147, arXiv:1208.0711 Jun Nishimura and A.T., PTEP 2013, 043B03, arXiv:1208.4910 arXiv: 1305.5547 Hajime Aoki, Jun Nishimura and A. T., in preparation Yuta Ito, Jun Nishimura and A. T., in preparation
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Present status of superstring theory
Numerous vacua
Cosmic (initial) singularity
space-time dimensionsgauge groupsmatter contents (generation number)
Liu-Moore-Seiberg (’02), ……
perturbation theory + D-brane
various
Use the statistical method or appeal to the anthropic principle
There are numerous vacua that are theoretically allowed
In general, perturbation theory cannot resolve the cosmic singularity
Non-perturbative effects are important at the beginning of the universe
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Matrix models
IIB matrix model Ishibashi-Kawai-Kitazawa-A.T. (’96)
Matrix theory Banks-Fischler-Shenker-Susskind (‘96)
Matrix string theory Dijkgraaf-Verlinde-Verlinde (’97)
10D U(N)SYM
0D
1D
2D
There is a possibility that one can actually determine the true vacuum uniquely and resolve the cosmic singularity if one uses a nonperturbative formulation that incorporates full nonperturbative effects.
We study the IIB matrix model. “Lorentzian” is a key to this project.
~ lattice QCD for QCDProposals
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Plan of the present talk
1. Introduction2. Review of the IIB matrix model3. Defining Lorentzian version4. SSB of SO(9) symmetry to SO(3)5. Realizing the Standard Model particles6. Summary and outlook
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IIB matrix model
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IIB matrix model
Space-time does not exist a priori, but is generated dynamicallyTime is given a priori in Matrix theory and matrix string theory
Manifest SO(9,1) symmetry, manifest 10D N=2 SUSY
: 10D Lorentz vector: 10D Majorana-Weyl spinor
Hermitian matrices
Large- limit is taken
covariant formulation Matrix theory and matrix string theory are light-cone formulation
Ishibashi-Kawai-Kitazawa-A.T. (’96)
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Correspondence with world-sheet action
Green-Schwarz action of Schild-type for type IIB superstrig with κ symmetry fixed
IIB matrix model
2nd quantized
matrix regularization
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eigenvalues of are coordinates
10D N=2 SUSY
dimensional reduction of 10D N=1 SUSY
10D N=2 SUSY
suggests that the model includes gravity
Corresponding to 10DN=2SUSY possessed by Green-Schwarz action
translation of eigenvalues
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Interaction between D-branes
graviton scalar
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Light-cone string field theory
Schwinger-Dyson equation for on the light front
light-cone string field theory for type IIB superstring
This implies that IIB matrix model reproduces perturbation theory of type IIB superstring
Fukuma-Kawai-Kitazawa-A.T. (’97)
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Euclidean model
Wick rotationEuclidean model
manifest SO(10) symmetry
Euclideanization
Krauth-Nicolai-Staudacher (’98), Austing-Wheater (’01)
Euclidean model is well-defined without cutoffs
People have been studying the Euclidean model
opposite sign ! looks quite unstable
Lorentzian model
: positive definite
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10 hermitian matrices
Space-time in Euclidean model
Aoki-Iso-Kawai-Kitazawa-Tada (’99)low energy effective theory for ~ branched polymer
10 D4 D
configurations diagonalizable simultaneously are favored
SSB of SO(10) to SO(4)
If eigenvalues are distributed on 4D hyperplane, SSB of SO(10) to SO(4) occurs ~ dynamical generation of 4D space-timeBut not confirmed so far
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Kim-Nishimura-A. T. (’11)
Defining Lorentzian version
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Why Lorentzian version? see time evolution of universe
~ need to study real time dynamics Wick rotation in gravitational theory seems nontrivial, in contrast to
field theory on flat space-time
ex.) causal dynamical triangulation ( CDT) Ambjorn-Jurkiewicz-Loll (’05)
Coleman mechanism in space-time with Lorenztian signature
Kawai-Okada (’11)
Recent results for the Euclidean model in Gaussian expansion method Nishimura-Okubo-Sugino (’11)
suggest dynamical generation of 3-dimensional space-time
Here we study Lorentzian version of the IIB matrix model
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Regularization and large-N limit
By introducing cutoffs, we make time and space directions finite
It turns out that these cutoffs can be removed in the large-N limit ~quite nontrivial dynamical property Lorentzian version is well-defined we expect the effect of the explicit breaking of SO(9,1) and SUSY due to the cutoffs to vanish in the large-N limit need to check
How to define partition functionnatural from a viewpoint of the Wick rotationof worldsheet
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Kim-Nishimura-A. T. (’11)
SSB of SO(9) to SO(3)
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average
Emergence of concept of ``time evolution”
represents space structure at fixed time t
We observe band-diagonal structure
small
small
these values are determined dynamically
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We take
Determination of block size
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SSB of SO(9) symmetry
“critical time”
SSB
symmetric under
we only show
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Exponential expansion
inflation
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From exponential to linear
6d bosonic model omit fermions
Big Bang?
inflation
radiation dominated universe
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Nishimura-A. T. (’12)Aoki-Nishimura-A. T., work in progress
Cf.) Chatzistavrakidis-Steinnacker-Zoupanos (’11)
Realizing Standard Model particles
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Late time behaviors
It is likely that we see the beginning of universe (inflation) in the present Monte Carlo simulation we need larger N to see late times At later times, ``well-known” universe should emerge
Do inflation and big bang occur?not phenomenological description by ``inflaton” but first principle description by superstring theory
The Standard Model should appear
present accelerating expansion (dark energy)understanding of cosmological constant problem
we can expect that at late times classical approximation is good and fluctuation around the background is small because the action is large due to expansion
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Chiral fermions
Dirac equation in 10d
is Majorana-Weyl in 10d
massless modes
chiral fermions in 4d
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and are different
Background
(3+1)d Lorentz symmetric backgroundmatrix analog of warp factor
# of zero modes with each chirality is the same
constructive definition
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Warped geometry and chiral fermion
# of variables < # of equationsno solution generically
we obtain left-handed chiral fermion in 4d
many solutions
warped geometry
vector-like fermions no-go theorem
direct product
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Example intersecting branes
4
5
6
6
5
9
7
4
8
~ D5-brane
~ D7-brane
fuzzy spheres
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Solving 6d Dirac equation
L
R
we solve
charge conjugation ~ identified
zero modes ( ) appear at intersection points ~ L and R
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Wave functions and warp factor
Left-handed
Right-handed
zero modes
1st excited state
we obtain one generation of left-handed fermion
6 4, 5
64, 5
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Three generations
R L R
LR
L
we squash
we obtain three generations of left-handed fermionswave functions are different among generations so are Yukawa coupling
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Standard Model fermions and right-handed neutrino Cf.) Chatzistavrakidis-Steinnacker-Zoupanos (’11)
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Summary and outlook
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when is made diagonal, have band-diagonal structure
Summary We studied Lorentzian version of the IIB matrix model
We introduced the infrared cutoffs and found that they can be removed in the large-N limit The model thus obtained is well-defined and has no parameters except one scale parameter
This property is expected in nonperturbative string theory the concept of ``time evolution” emerges
After a critical time, SO(9) symmetry of 9 dimension is spontaneously broken down to SO(3) and 3 out of 9 dimensions start to expand rapidly ~ can be interpreted as birth of universe
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Summary (cont’d)
We gave an example of background where three generations of the Standard Model particles are realized
We found that matrix analog of warp factor must be introduced to realize chiral fermions, and gave an example of background yielding the chiral fermion
We confirm that the expansion is exponential ~ beginning of inflation We observe transition from exponential expansion to linear one in toy model
There is a possibility that Standard Model can be derived uniquely at low energy structure of extra dimensions and warp factor are determined dynamically ~ to substantiate string theory
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Outlook
background at late time : e-foldings, Big Bang, Standard Model
use the idea of renormalization group to reach the late time ~ work for a toy model
It is important to study the classical solutions and look for a solution connected smoothly to the simulation Kim-Nishimura-A. T. (’12)
more efficient Monte Carlo simulation ~ parallelization
calculation of Yukawa couplings : mass hierarchy , CKM matrix and
MNS matrix
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Outlook (cont’d)
Does exponential expansion occur? Does big bang occur after that? it should be seen as (the second) phase transition Does it occur at the same time as commutative space-time appears How density fluctuation can be measured to compare with CMB Can lagrangian of GUT be read off from fluctuation around the classical solution? Does standard model appear at low energy? We expect to understand in a unified way various problems in particle physics and cosmology such as mechanism of inflation, cosmological constant problem, hierarchy problem, dark matter, dark energy, baryogenesis
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String duality
Het SO(32)
Het E8 x E8
M
IIA
IIB
I
dualities in superstring theory
five superstring theories and M theory are different descriptions of one theory
One can start everywhere with a formulation which enables one to treat strong coupling dynamics
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How to define partition function
natural from a viewpoint of correspondencewith worldsheet theory
Wick rotation for worldsheet
Lorentzian version
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unlike the case of the Euclidean model, the Lorentzian model is ill-defined as it stands
By introducing cutoffs, we make time and space directions finite
It turns out that these cutoffs can be removed in the large-N limit ~quite nontrivial dynamical property SO(9,1) symmetry and SUSY are explicitly broken by the cutoffs we expect the effect of the explicit breaking to vanish in the large-N limit need to check
without loss of generalitywe put
Regularization and large-N limit
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(1) Pfaffian coming from integral over fermion
in the Euclidean model
is dominant in the large-N limit
can give rise to sign problem
(2) (1)
Avoiding sign problem
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(2) How to treat
homogeneousin
first perform
Also problem in field theory on Minkowski space( analysis of real time dynamics is a notorious problem )
Avoiding sign problem (cont’d)
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Time evolution of space size
peak at starts to grow for
Symmetric under
We only show
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Late time behaviors
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Seeing later times
It is likely that we see the beginning of universe in the present Monte Carlo simulation At later times, ``well-known” universe should emerge
Do inflation and big bang occur?not phenomenological description by ``inflaton” but first principle description by superstring theory
can be tested by comparison with CMB How commutative space-time appears
What massless fields appear on it
present accelerating expansion (dark energy)understanding of cosmological constant problem
prediction for fate of universe big crunch or big rip
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Classical approximation as a complementary approach
if we reach the time by Monte Carlo simulation and uniquely pick up a dominant classical solution connected smoothly to the result in the simulation, we can study late time behaviors
we expect classical approximation is good after late times because action becomes large due to expansion
there are infinitely many solutions
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variation function
EOM
Example of solution
SL(2,R) solution
(3+1)-dimensional space-time ~ R×S3
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identify t0 with the present time
present accelerating expansion
cosmological constant ~ solve cosmological constant problem
cosmological constant term vanishes in the future
considered to give late time behaviors in the matrix model
Cosmological implication of SL(2,R) solution
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Chiral fermions cont’d
nonzero eigenvalues are paired
finite-N matrices ~space of with each chirality has the same dimensions ~number of zero modes with each chirality is the same
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Commutative space-time and local fields
results in Monte Carlo simulation
are smaller than
there are classical solutions representing (3+1)-dimensional commutative space-time
we assume a classical solution representing (3+1)-dimensional
commutative space-time is dominant at sufficiently late timesare close to diagonal
space-time points in 3+1 dimensions
are small for with
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Commutative space-time and local fields (cont’d)
fluctuations around the classical solution
we further assume that fluctuations corresponding to massless modes are also close to diagonal
are close to each other
same structure in cubic and quartic tems
local field theory
In arXiv:1208.4910, we showed that NG modes for symmetry breaking of Poincare symmetry and SUSY indeed appear as local massless fields
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is also a classical solution
cf.) Iso-Kawai (’99)
if are a classical solution,
fluctuations around
c.f.) stack of k D-branes SU(k) gauge theory
Gauge symmetry
local SU(k) symmetry
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is a linear combination of
3 2 1 1 1
: mirror partners
: bi-fundamental rep. of
hypercharge can be assigned consistently
minimum
c.f.) H.Aoki PTP 125 (2011) 521 Chatzistavrakidis-Steinacker-Zoupanos JHEP 09 (2011) 115
GUT
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Given a classical solution, we can read off detail of local field theory from fluctuations around it ~ GUT
Is there a classical solution that allows chiral fermions?
Is part of SUSY preserved? (we can answer this question if we are given the classical solution) if this is the case, hierarchy problem is OK if this is not, all scalar fields acquire mass of GUT scale due to radiative correction composite Higgs structure of extra dimension in the classical solution is important
c.f.) H.Aoki PTP 125 (2011) 521 Chatzistavrakidis-Steinacker-Zoupanos JHEP 09 (2011) 115
GUT (cont’d)
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Summary (cont’d)
We gave a general prescription to find solutions and classified the solutions under some ansatzes We gave a general prescription to find solutions and classified the solutions under some ansatzes
We found a solution which represents expanding (3+1)-dimensional
universe and resolves cosmological constant problem
To reach late times, we need larger N, while Classical approximation should be good at late times There are infinitely many solutions we need to know which one is smoothly connected to MC result
Kim-Nishimura-A. T. (’12)