quantum avoidance of the big rip singularity in eddington-inspired-born-infeld theory ·...
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Quantum avoidance of the big rip singularityin Eddington-inspired-Born-Infeld theory
Che-Yu Chen
Institute of physics, National Taiwan UniversityLeCosPA, National Taiwan University
Work done under the supervision of Dr. M. Bouhmadi-Lopez (Universidade da BeiraInterior (Portugal)) and Prof. Pisin Chen (NTU and Standford University)
5th Dec. 2016
Che-Yu Chen (National Taiwan University) 05-12-2016 1 / 33
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References
Eur. Phys. J. C 74, 2802 (2014), arXiv:1302.5013
M. Bouhmadi-Lopez, C-Y- Chen and P. Chen
Eur. Phys. J. C 75, 90 (2015), arXiv: 1406.6157
M. Bouhmadi-Lopez, C-Y- Chen and P. Chen
JCAP 1611, no. 11, 023 (2016), arXiv:1609.00700
M. Bouhmadi-Lopez and C-Y- Chen
Che-Yu Chen (National Taiwan University) 05-12-2016 2 / 33
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Outline
1 Introduction
2 Big Rip in the EiBI theory
3 Quantization of the EiBI theoryStandard approach: Start from the actionA “phenomenological” approach: Start from the Friedmann equations
4 Conclusion
Che-Yu Chen (National Taiwan University) 05-12-2016 3 / 33
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Outline
1 Introduction
2 Big Rip in the EiBI theory
3 Quantization of the EiBI theoryStandard approach: Start from the actionA “phenomenological” approach: Start from the Friedmann equations
4 Conclusion
Che-Yu Chen (National Taiwan University) 05-12-2016 4 / 33
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Introduction-1-: motivation
Einstein general relativity (GR) is an extremely successful theory for
more than a century
There are some motivations for looking for possible extension of GR:
singularity at high energies, late time acceleration...
To explain the acceleration, some kinds of Dark Energy or
modifications are needed: C.C, quintessence, Generalized Chaplygin
Gas(GCG), phantom...
More singularities?
Che-Yu Chen (National Taiwan University) 05-12-2016 5 / 33
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Big Rip
Caldwell, Kamionkowski, Weinberg (2003)
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Introduction-2-: motivation
Born-Infeld action for electrodynamics in 1934:√|gµν + κFµν |
Theories of gravity with Born-Infeld determinantal action have been
widely investigated:√|gµν + κGµν |
S. Deser and G. W. Gibbons (1998)
BUT most of them suffer from ghost instability (pure metric
formalism)
An alternative Born-Infeld determinantal theory within Palatini
formalism has been proposed - Eddington-inspired-Born-Infeld gravity
Banados, Ferreira (2010)
Che-Yu Chen (National Taiwan University) 05-12-2016 7 / 33
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The theory-1-:
SEiBI(g , Γ,Ψ) = 2κ
∫d4x
[√|gµν + κRµν(Γ)| − λ
√−g]
+ Sm(g ,Ψ)
Palatini formalism: g , Γ, Sm(g ,Ψ)
The compatibility: Γ⇔ qµν ≡ gµν + κRµν
No torsion T = 0
κ is the only parameter characterizing the theory (8πG = c = 1)
λ is related to the cosmological constant Λ
Recover GR+C.C at low curvature limit
Sg ≈ 12
∫d4x√−g[R − 2(λ−1)
κ
]
Che-Yu Chen (National Taiwan University) 05-12-2016 8 / 33
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The theory-2-:
SEiBI(g , Γ,Ψ) = 2κ
∫d4x
[√|gµν + κRµν(Γ)| − λ
√−g]
+ Sm(g ,Ψ)
A radiation dominated universe: Big Bang is avoided through aLoitering effect if κ > 0
a→ al when t → −∞The Big Bang is substituted by a bounce if κ < 0
5 10 15 20t
1
2
3
4
5a�al
-2 -1 1 2 3 4ΚΡ
-0.3
0.3ΚH2
Banados, Ferreira (2010)
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Outline
1 Introduction
2 Big Rip in the EiBI theory
3 Quantization of the EiBI theoryStandard approach: Start from the actionA “phenomenological” approach: Start from the Friedmann equations
4 Conclusion
Che-Yu Chen (National Taiwan University) 05-12-2016 10 / 33
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The EiBI scenario and the Big Rip
We consider an EiBI universe (κ > 0) filled with radiation, matter
and, a phantom dark energy component with a constant equation of
state w < −1
The physical metric gµν : a→∞, ρ→∞
H2 ≈ 4√|w |3
3(3w+1)2 ρ→∞, and dHdt ≈
2√|w |3
(3w+1)2 |1 + w |ρ→∞ at a finite t
(Big Rip)
For the same w , the singular event is slightly postponed in the EiBI
theory compared with GR
M. Bouhmadi-Lopez, C. Y. Chen, P. Chen (2014),(2015)
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The evolution of a bound structure near Big Rip
The evolution of a bound system can be estimated by
r =a
ar − GM
r2+
L2
r3, r2φ = L
S. Nesseris, L. Perivolaropoulos (2004)
Near the singularity:
r(t) = A1(tmax − t)2
3(1+w) + A2(tmax − t)1− 23(1+w) ,
φ(t) ≈ 3(w+1)1−3w
LA1
2 (tmax − t)3w−1
3(w+1) + φ0
M. Bouhmadi-Lopez, C. Y. Chen, P. Chen (2015)
Che-Yu Chen (National Taiwan University) 05-12-2016 12 / 33
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The EiBI scenario and the Big Rip
The geometry corresponding to the connection (or qµν)
The auxiliary metric qµν (t → t, a→ a, so that qµν = [−1, a2δij ]):
Hq2 ≡ ( 1
adadt
)2 → 13κ , and a ∝ eHq t when t →∞ (de-Sitter)
Does not couple to matter (observers)
M. Bouhmadi-Lopez, C. Y. Chen, P. Chen (2015)
Che-Yu Chen (National Taiwan University) 05-12-2016 13 / 33
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The full analysis of EiBI phantom model
Singularity in GR EiBI physical metric EiBI auxiliary metric
Big Rip Big Rip expanding de-Sitter
past Sudden past Type IV (0 < α ≤ 2) contracting de-Sitter
(α > 0) past Sudden (α > 2)
future Big Freeze future Big Freeze (−3 < α < −1) expanding de-Sitter
(α < −1) future Type IV (α = −3)
future Sudden (α < −3)
past Type IV past Sudden (−2/3 < α < −1/3) past Type IV
(−1 < α < 0) (1)past Type IV
(α 6= −n/(n + 1)) (2)finite past without singularity finite past without singularity
past loitering effect (ab > amin) Big Bang
finite past without singularity finite past without singularity finite past without singularity
(α = −n/(n + 1))
(−1 < α < 0)
past loitering effect (ab > amin) Big Bang
Little Rip Little Rip expanding de-Sitter
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Outline
1 Introduction
2 Big Rip in the EiBI theory
3 Quantization of the EiBI theoryStandard approach: Start from the actionA “phenomenological” approach: Start from the Friedmann equations
4 Conclusion
Che-Yu Chen (National Taiwan University) 05-12-2016 15 / 33
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Quantizing EiBI theory? Why?
The big rip singularity is still unavoidable in the EiBI theory→ The theory is still NOT complete
Some quantum effects are expected near the classical big ripsingularity
Quantum avoidance of the DE singularities in GR
The quantization of theories constructed upon Palatini formalism:(g , Γ)
Some results which are model-independent? Further step to quantumgravity?
Che-Yu Chen (National Taiwan University) 05-12-2016 16 / 33
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Quantizing EiBI theory? How?
FLRW ansatz → Quantum cosmology
Quantum Geometrodynamics → Wheeler DeWitt (WDW) equationHΨ = 0
The DeWitt condition: Ψ→ 0singularity avoidance
Does it sufficiently imply a vanishing probability? NO
A potential hint for singularity avoidance
B. S. DeWitt (1967)
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Outline
1 Introduction
2 Big Rip in the EiBI theory
3 Quantization of the EiBI theoryStandard approach: Start from the actionA “phenomenological” approach: Start from the Friedmann equations
4 Conclusion
Che-Yu Chen (National Taiwan University) 05-12-2016 18 / 33
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How to start? The alternative action
SEiBI = 2κ
∫d4x
[√|gµν + κRµν(Γ)| − λ
√−g]
+ Sm(g ,Ψ)
The problematic square root√...
It may be possible to use Lagrangian multipliers → too many variables
An alternative action which is dynamically equivalent!!
T. Delsate, J. Steinhoff (2012)
Sa = λ∫d4x√−q[R(q)− 2λ
κ + 1κ
(qαβgαβ − 2
√gq
)]+ Sm(g ,Ψ)
{g ,Γ}→{g ,q}Linear on R(q) ≡ qαβRβα(q) (like SEH)
q → dynamical g → non-dynamical
The field equations are exactly the SAME!!
T. Delsate, J. Steinhoff (2012)
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FLRW universe
The FLRW ansatz
gµνdxµdxν = −N(t)2dt2 + a(t)2d~x2,
qµνdxµdxν = −M(t)2dt2 + b(t)2d~x2.
Perfect fluid assumption→
L = λMb3[− 6b2
M2b2− 2λ
κ+
1
κ
(N2
M2+ 3
a2
b2− 2
Na3
Mb3
)]− 2ρ(a)Na3
E.O.M
N: gauge fixing M: Firedmann eq. of b
a: relating a and b b: Rauchaudhuri eq. of b
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Constructing the Hamiltonian H
Conjugate momenta:
pb =∂L∂b
= −12λb
Mb
The Hamiltonian
H = M[−
p2b
24λb+
2λ2
κb3 +
1
κλ(λ+ κρ(a))2 a
6
b3− 3λ
κba2]
Canonical quantization: {a, b, pb} → Operators → Quantum level
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The first factor ordering: The WDW equation
b3H = 0→[∂2
∂x2 + V1(a, x)]Ψ(a, x) = 0, x = ln(
√λb)
V1(a, x) =24
κ~2
[2e6x − 3a2e4x + (λ+ κρ(a))2a6
]WKB approximation: If V1 → +∞ when a→∞, then Ψ→ 0
Ψ(a, x) ≈ V1(a, x)−14 exp
{± i
∫ x√V1(a, x ′)dx ′
}Goal: To prove V1 → +∞ when a→∞ for all x
M. Bouhmadi-Lopez, C. Y. Chen (2016)
Che-Yu Chen (National Taiwan University) 05-12-2016 22 / 33
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First factor ordering: Ψ→ 0 when a→∞
V1(a, x) = 24κ~2 e
6x [2− 3δ + (λ+ κρ(a))2δ3] δ ≡ a2e−2x ∝ a2/b2
If when a→∞....
δ → 0 (a� b →∞): the −3δ term can be neglectedδ →∞ (a� b):
V1(a, x) ≈ 24
κ~2(λ+ κρ(a))2a6
δ → finite constant (a ≈ b):
V1(a, x) ≈ 24
κ~2(λ+ κρ(a))2a6
V1 → +∞ when a→∞ for all x!! Ψ→ 0
M. Bouhmadi-Lopez, C. Y. Chen (2016)
Che-Yu Chen (National Taiwan University) 05-12-2016 23 / 33
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First factor ordering: Ψ→ 0 when a→∞
A guiding example: If a and b are related through E.O.Mand p = wρ (w < −1)
Without WKB approximation:
Ψ(x) = C1J0(A1e3x) + C2Y0(A1e
3x) A1 ≡4√
3κ~2
When x →∞ (as well as a)
Ψ(x) ≈√
2
πA1e−3x/2
[C1 cos
(A1e
3x − π
4
)+ C2 sin
(A1e
3x − π
4
)]M. Bouhmadi-Lopez, C. Y. Chen (2016)
Che-Yu Chen (National Taiwan University) 05-12-2016 24 / 33
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Second factor ordering: The WDW equation
H = 0→[∂2
∂y2 + V2(a, y)]Ψ(a, y) = 0, y ≡ (
√λb)3/2
Similar strategy...
V2(a, y) =32
3κ~2y2[2−3η+(λ+κρ(a))2η3
]η ≡ a2y−4/3 ∝ a2/b2
WKB approximation: If V2 → +∞ when a→∞, then Ψ→ 0
Ψ(a, y) ≈ V2(a, y)−14 exp
{± i
∫ y √V2(a, y ′)dy ′
}M. Bouhmadi-Lopez, C. Y. Chen (2016)
Che-Yu Chen (National Taiwan University) 05-12-2016 25 / 33
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Second factor ordering: Ψ→ 0 when a→∞
V2(a, y) = 323κ~2 y
2[2− 3η + (λ+ κρ(a))2η3
]η ≡ a2y−4/3 ∝ a2/b2
If when a→∞....
η → 0 (a� b →∞):
η →∞ (a� b):
η → finite constant (a ≈ b):
V2 → +∞ when a→∞ for all y !! Ψ→ 0
M. Bouhmadi-Lopez, C. Y. Chen (2016)
Che-Yu Chen (National Taiwan University) 05-12-2016 26 / 33
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Second factor ordering: Ψ→ 0 when a→∞
A guiding example: If a and b are related through E.O.Mand p = wρ (w < −1)
Without WKB approximation:
Ψ(y) = C1√yJ1/4(A1y
2) + C2√yY1/4(A1y
2)
When y →∞ (as well as a)
Ψ(y) ≈
√2
πA1y
[C1 cos
(A1y
2 − 3π
8
)+ C2 sin
(A1y
2 − 3π
8
)]M. Bouhmadi-Lopez, C. Y. Chen (2016)
Che-Yu Chen (National Taiwan University) 05-12-2016 27 / 33
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Outline
1 Introduction
2 Big Rip in the EiBI theory
3 Quantization of the EiBI theoryStandard approach: Start from the actionA “phenomenological” approach: Start from the Friedmann equations
4 Conclusion
Che-Yu Chen (National Taiwan University) 05-12-2016 28 / 33
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The “phenomenological” Wheeler DeWitt equation
A phenomenological WDW equation from the Friedmann equations
κH2 ≈4√|w |3
3(3w + 1)2a−3(1+w) κH2
q = κ(1
b
db
dt
)2≈ 1
3
t = rescaled time
HtΨ(a, b) = HgHqΨ(a, b) = 0 Ψ(a, b) = ψ1(a)ψ2(b)
c.f. The direct product of two independent spaces( d2
da2+
48√|w3|
κ~2(3w + 1)2a4+ε
)ψ1(a)
( d2
db2+
12
κ~2b4)ψ2(b) = 0
M. Bouhmadi-Lopez, C. Y. Chen (2016)
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The vanishing of the wave function(d2
da2 +48√|w3|
κ~2(3w+1)2 a4+ε)ψ1(a)
(d2
db2 + 12κ~2 b
4)ψ2(b) = 0
Two possibilities:(d2
da2 +48√|w3|
κ~2(3w+1)2 a4+ε)ψ1(a) = 0
(d2
db2 + 12κ~2 b
4)ψ2(b) = K1(b)
or...(d2
da2 +48√|w3|
κ~2(3w+1)2 a4+ε)ψ1(a) = K2(a)
(d2
db2 + 12κ~2 b
4)ψ2(b) = 0
K1 and K2 are bounded functions
In both cases, ψ1(a)→ 0 when a→∞ and ψ2(b) is bounded for all b
Ψ(a, b) = ψ1(a)ψ2(b)→ 0 when a→∞ for all b
M. Bouhmadi-Lopez, C. Y. Chen (2016)
Che-Yu Chen (National Taiwan University) 05-12-2016 30 / 33
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Outline
1 Introduction
2 Big Rip in the EiBI theory
3 Quantization of the EiBI theoryStandard approach: Start from the actionA “phenomenological” approach: Start from the Friedmann equations
4 Conclusion
Che-Yu Chen (National Taiwan University) 05-12-2016 31 / 33
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Conclusion
The big rip singularity is unavoidable in the EiBI theory, even though
most singularities can be alleviated in it
The bound structures would be ripped apart before the singularity
Quantum geometrodynamics within EiBI framework - quantum
cosmology
Standard approach: An alternative action → Lagrangian → H→WDW eq. (two factor ordering)
Phenomenological approach: Two Friedmann eqs. → Ht → WDW eq.
DeWitt condition is satisfied → big rip is expected to be avoided in
quantum level
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Conclusion
Thank you for your attention:)
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