cosmological implications of the group field theory …kcl...cosmological implications of the group...
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Cosmological implications of the group field theory approach
to quantum gravityMarco de Cesare
King’s College Londonin collaboration with D.Oriti, A.Pithis, M.Sakellariadou:
MdC,MS: Phys.Lett. B764 (2017) 49-53, ArXiv:1603.01764 MdC,AP,MS: Phys.Rev. D94 (2016) no.6, 064051, ArXiv:1606.00352
MdC,DO,AP,MS: ArXiv: 1709.00994
COST training school: “Quantum Spacetime and Physics Models” Corfu, Greece, 16-23 September 2017
2
• Emergent cosmology scenario in group field theory (GFT)
• Some brief remarks on GFT
• Effective Friedmann dynamics
• Cosmological implications of GFT models
• No interactions between quanta
• Interactions are allowed
• Anisotropies in the EPRL model
• Conclusions
Plan of the Talk
Group Field Theory (GFT)• GFT is a non-perturbative and background
independent approach to Quantum Gravity (Oriti ’11, ’13)
• Fundamental degrees of freedom are discrete objects carrying pre-geometric data (holonomies, fluxes)
• The dynamics of the GFT is obtained from a path-integral
• The interaction potential contains the information about the gluing of quanta to form 4D geometric objects.
Z =
Ze�S['] S = K + V
Figures: Gielen,Sindoni ‘16
4
• Quantum spacetime as a many-body system
• Spacetime is an emergent concept, determined by the collective dynamics of ‘quanta’ of geometry
• Cosmological background obtained by considering the dynamics of a condensates of such ‘quanta’ (Gielen,Oriti,Sindoni ’13)
• Evolution is defined in a relational sense (matter clock )
Cosmology from GFT
Main advantages• Cosmology can be obtained from the full theory
• The formalism naturally allows for a varying number of ‘quanta’
• It may offer a way to go beyond standard cosmology
�
5
• mean field
• spin representation
• Enforce isotropy (tetrahedra have equal faces)
• Homogeneous and isotropic background can be studied by looking at the expectation value of the volume operator
Cosmological Background
V (�) =X
j
Vj |�j(�)|2 Vj ⇠ j3/2`3Pl
' = '(g1, g2, g3, g4;�)
'j1,j2,j3,j4,◆(�)
�j(�) = 'j,j,j,j,◆?(�)
gi 2 SU(2)
6
• The dynamics of yields effective equations for the evolution of
• Simplification obtained when restricting to one spin j
• Last assumption is justified by results concerning the emergence of a low-spin phase (Gielen’16) (Pithis,Sakellariadou,Tomov’16)
Emergent Friedmann dynamics�j
V
@�V
V= 2
@�⇢
⇢
@2�V
V= 2
"@2�⇢
⇢+
✓@�⇢
⇢
◆2#
@�V
V=
2P
j Vj⇢j@�⇢jPj Vj⇢2j
(Oriti,Sindoni,Wilson-Ewing ’16)
⇢j = |�j |
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• Single spin effective action (index j dropped)
• Global U(1) conserved charge , interpreted as the momentum canonically conjugated to
• Polar decomposition of the mean field
• Equation of motion of the radial part
Effective Friedmann equation
Seff =
Zd�
�A |@��|2 + V(�)
�
The non-interacting case
�⇡� = a3�
Q
V(�) = B|�(�)|2
� = ⇢ ei✓ Q ⌘ ⇢2@�✓
@2�⇢�
Q2
⇢3� B
A⇢ = 0 E = (@�⇢)
2 +Q2
⇢2� B
A⇢2
(Oriti,Sindoni,Wilson-Ewing ’16)(MdC,Sakellariadou ’16)
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• The effective Friedmann equation can be recast in the form
• The effective gravitational constant can be computed exactly in the free model
• In the large volume limit one recovers the ordinary Friedmann evolution
• There is a bounce when . This takes place when
Bouncing Universe
H2 =8⇡Geff
3", " =
�2
2
Geff (�) =G�E2
+ 12⇡GQ2�sinh
2⇣2
p3⇡G(�� �)
⌘
⇣E �
pE2
+ 12⇡GQ2cosh
⇣2
p3⇡G(�� �)
⌘⌘2 .
� ! 1
Geff = 0 (at � = �)H2 = 0
(MdC,Sakellariadou ’16)
(a = V 1/3)
Bouncing Universe
-4 -2 2 4ϕ
0.2
0.4
0.6
0.8
1.0
Geff
-4 -2 2 4ϕ
0.2
0.4
0.6
0.8
1.0
1.2
1.4Geff
E<0 E>0
profile of for opposite signs of the conserved charge E. The behaviour is generic for Q 6= 0
Geff
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• An early era of accelerated expansion is usually assumed in order to solve the classic cosmological puzzles.
• We seek a relational definition of the acceleration
• Classically, for a minimally coupled scalar field, we have:
Accelerated expansion (geometric inflation)
a
a=
1
3
⇣⇡�
V
⌘2"@2�V
V� 5
3
✓@�V
V
◆2#
(a = V 1/3)
Accelerated expansion
0.5 1.0 1.5 2.0 2.5 3.0ϕ
2
4
6
8
0.5 1.0 1.5 2.0 2.5 3.0ϕ
1
2
3
4
5
6
7
E<0 E>0
a
a=
1
3
⇣⇡�
V
⌘2"@2�V
V� 5
3
✓@�V
V
◆2#
N =
1
3
log
✓Vend
Vbounce
◆=
2
3
log
✓⇢end
⇢bounce
◆number of e-folds
too small in the free caseN ⇠ 0.1
(MdC,Sakellariadou ’16)
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• The role of interactions in GFT is crucial for two main reasons: • Interactions prescribe the gluing of quanta to form 4D geometric
objects
• They have important consequences for cosmology
• Phenomenological approach
The impact of interactions
Seff =
Zd�
�A |@��|2 + V(�)
�
V(�) = B|�(�)|2 + 2
nw|�|n +
2
n0w0|�|n
0w0 > 0, A,B < 0
(MdC,Pithis,Sakellariadou ’16)
�(ϕ)��
0.0 0.5 1.0 1.5 2.0 2.5
50
100
150
200
ϕ
13
Cosmological evolution is periodic. Endless sequence of expansions and contractions, matched with bounces
Cyclic Universe
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Number of e-folds: switching on the interactions
log(�) log(-�)
10 20 30 40 50 60 70
50
100
150
200
250
300
������ �� �-�����
���(�)
0.2 0.4 0.6 0.8 1.0
1.0
1.5
2.0
2.5
3.0
3.5
������ �� �-�����
log(�) log(-�)
59.5 60.0 60.5 61.0
260
265
270
275
������ �� �-�����V(�) = B|�(�)|2 + 2
nw|�|n +
2
n0w0|�|n
0
(MdC,Pithis,Sakellariadou ’16) No intermediate deceleration stage
N =
2
3
log
✓⇢end
⇢bounce
◆
15
Number of e-folds: switching on the interactions
log(�) log(-�)
10 20 30 40 50 60 70
50
100
150
200
250
300
������ �� �-�����
(MdC,Pithis,Sakellariadou ’16)
can be arbitrarily large!N
Bonus
n0 > n
n � 5
Constraints:
w < 0
V(�) = B|�(�)|2 + 2
nw|�|n +
2
n0w0|�|n
0
N =
2
3
log
✓⇢end
⇢bounce
◆
• GFT for the EPRL model
• Perturb the isotropic background
Microscopic anisotropiesS = K + V5 + V 5
' = '0 + �'
g2, j2
g1, j1
g3, j3
g4, j4
-2 -1 0 1 2
1.0
1.2
1.4
1.6
1.8
2.0
ϕ
A
V
area-to-volume ratio
V =1
5
Zd�
X
ji,mi,◆a
'j1j2j3j4◆1m1m2m3m4
'j4j5j6j7◆2�m4m5m6m7
'j7j3j8j9◆3�m7�m3m8m9
'j9j6j2j10◆4�m9�m6�m2m10
'j10j8j5j1◆5�m10�m8�m5�m1
(MdC,Oriti,Pithis,Sakellariadou ’17)
⇥10Y
i=1
(�1)ji�mi V5(j1, . . . , j10; ◆1, . . . ◆5)
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Within the GFT framework, homogeneous and isotropic cosmologies are described as coherent states of basic building blocks.
Our results:
• Bouncing cosmologies are a generic feature of the theory
• Interactions between quanta lead to a cyclic Universe
• Suitable choices of the interactions can make the early Universe accelerate for an arbitrarily large number of e-folds
• Anisotropies decay away from the bounce in a region of parameter space
Conclusions
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• MdC,Sakellariadou’16: "Accelerated expansion of the Universe without an inflaton and resolution of the initial singularity from Group Field Theory condensates", arXiv:1603.01764
• MdC,Pithis,Sakellariadou’16: “Cosmological implications of interacting Group Field Theory models: cyclic Universe and accelerated expansion", arXiv:1606.00352
• MdC,Oriti,Pithis,Sakellariadou’17: “Dynamics of anisotropies close to a cosmological bounce in quantum gravity", arXiv:1709.00994
• Oriti’11: “The microscopic dynamics of quantum space as a group field theory”, arXiv:1110.5606
• Oriti’13: “Group field theory as the 2nd quantization of Loop Quantum Gravity", arXiv:1310.7786
• Gielen,Oriti,Sindoni’13: “Cosmology from Group Field Theory Formalism for Quantum Gravity", arXiv:1303.3576
• Oriti,Sindoni,Wilson-Ewing’16: “Bouncing cosmologies from quantum gravity condensates", arXiv:1602.08271
• Gielen’16: “Emergence of a low spin phase in group field theory condensates", arXiv:1604.06023
References
EXTRAS
200 2 4 6 8 10 12 14
-1000
-500
0
500
ρ
U(ρ)
n=4, n'=5, λ=-1, μ=0.1, Q2=10, m2=10
0 2 4 6 8 10 12 14-60
-40
-20
0
20
40
60
ρ
ρ′
• Polar decomposition:
• Dynamics of the radial part:
Dynamics in the interacting model
� = ⇢ ei✓
@2�⇢ = �@⇢U
U(⇢) = �1
2m2⇢2 +
Q2
2⇢2+
�
n⇢n +
µ
n0 ⇢n0
E =1
2(@�⇢)
2 + U(⇢)
Q ⌘ ⇢2@�✓
and conserved quantities
E Q
� = �w
Aµ = �w0
A> 0with:
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Effective Friedmann equation (including interaction terms)
H2 =8Q2
9
"ma6
+"Ea9
+"Qa12
+"µ
a9�32n
�
"m =B
2A"E = VjE"Q = �Q2
2V 2j "µ = � w
nAV 1�n/2j
• Quantum gravity corrections • Compare with ekpyrotic models