Ginzburg-Landau theory of dark energyphysics.ipm.ac.ir/conferences/CGC/note/A.Banihashemi.pdf ·...
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Ginzburg-Landau theory of dark energy Abdolali Banihashemi In collaboration with Nima Khosravi, AmirHossein Shirazi Based on arXiv:1810.11007 NGC97, IPM . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .
Transcript of Ginzburg-Landau theory of dark energyphysics.ipm.ac.ir/conferences/CGC/note/A.Banihashemi.pdf ·...
Ginzburg-Landau theory of dark energy
Abdolali BanihashemiIn collaboration with
Nima Khosravi, AmirHossein ShiraziBased on arXiv:1810.11007
NGC97, IPM
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ΛCDM, Standard Model of Cosmology
Homogeneity, Isotropy & Spatially Flatness
→ ds2 = dt2 − a2(t)(dx2 + dy2 + dz2)
GR: Gµν = 8πGTµν + C .C . → Friedmann Eqs. and late timeacceleration.
Very simple initial conditions from Inflation: P(k) ∝ Akns−1
Abdolali Banihashemi Ginzburg-Landau theory of dark energy
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ΛCDM, Standard Model of Cosmology
With a few number of parameters, it matches well with data points!
Planck 2018.
Abdolali Banihashemi Ginzburg-Landau theory of dark energy
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Something is wrong here!
Abdolali Banihashemi Ginzburg-Landau theory of dark energy
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Something is wrong here!
Planck 2018
Abdolali Banihashemi Ginzburg-Landau theory of dark energy
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Something is wrong here!
Planck 2018
Abdolali Banihashemi Ginzburg-Landau theory of dark energy
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Something is wrong here!
Bourboux et al. 2017
Abdolali Banihashemi Ginzburg-Landau theory of dark energy
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Exploring the space of ideas. . .
These are all ”temporal” tensions;
. . . so maybe a ”phase transition” has occurred and weshould consider it!
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Ginzburg-Landau theory
Just care about symmetries. . .
L =
∫dd rL =
∫dd r
[C+
1
2m2tΦ2(r)+ξΦ3(r)+λΦ4(r)+γ(∇Φ(r))2+ζH(r)Φ(r)+. . .
]
t ≡ T − Tc
Tc
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Ginzburg-Landau Theory of Dark Energy
Λ = VGLTofDE (ϕ)
Zeroth order approximation
T − Tc ∝ z − zc
VGLTofDE = Λ1 +12m
2 z−zczc
ϕ2 + ξϕ3 + λϕ4
T>T c T<T cV (Φ)
Φ
Λ1
Λ2
δΛR
δΛL
A
BB
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Ginzburg-Landau Theory of Dark Energy
Λ(z) = Λ1X (z)
X (z) = 1 + A[tanh(α(z − zc)) + tanh(αzc)]
Λ(z)
z
H2(z) = H20
[Ωr (1+z)4+Ωm (1+z)3+Ωk (1+z)2+ΩΛ X (z)
]Ωr +Ωm +Ωk +ΩΛ = 1
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GLTofDE: results
0.32 0.16k
0.64
0.72
0.8
0.88
z t
0.3
0.6
0.9
1.2
A
0.27
0.3
m
69.0 70.5 72.0 73.5 75.0H0
0.32
0.16
k
0.64 0.72 0.80 0.88zt
0.3 0.6 0.9 1.2A
0.27 0.30m
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GLTofDE: results
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GLTofDE: results
Abdolali Banihashemi Ginzburg-Landau theory of dark energy
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GLTofDE: results
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A comment on negative Ωk
We could avoid this by letting ρΛ change its sign and get negative.This is what people do in reconstructing H(z). But it doesn’t seem
physical: ρDE (a) = ρ0DE exp
[ ∫ 1a da′3(1 + wDE (a
′))/a′]
Zhao 2018
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Beyond zeroth approximation
We can go beyond zeroth approximation by keeping the (∇Φ)2
and Φ3 terms in effective potential. Doing so will result insituation like this:
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Spatial anomalies of CMB
Surprisingly, CMB suffers from hemisphere asymmetry,quadrupole-octopole alignment and their orthogonality to dipolemode.
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Spatial anomalies of CMB
And cold spot!
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Beyond zeroth approximation of GLTofDE
We can address spatial anomalies of CMB in late timecosmology.
DE patches and Sachs Wolfe effect.
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Thank you!
Abdolali Banihashemi Ginzburg-Landau theory of dark energy
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GLTofDE and CMB spatial anomalies
We need a lot of simulations for taking care of patches’ sizedistribution.
Abdolali Banihashemi Ginzburg-Landau theory of dark energy
