GRAVITATIONALWAVES FROM/AFTER...
Transcript of GRAVITATIONALWAVES FROM/AFTER...
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GRAVITATIONAL WAVESFROM/AFTER REHEATING
DANIEL Ga FIGUEROADpto. Fısica Teorica UAM & Instituto de Fısica Teorica UAM-CSIC
GARCIA-BELLIDO & DGF, PRL 2007GARCIA-BELLIDO, DGF & SASTRE, PRD 2008
FENU, DGF, DURRER & GARCIA-BELLIDO, JCAP 2009DUFAUX, DGF & GARCIA-BELLIDO, PRD 2010
BENASQUE 2010, August 17th 2010, SPAIN
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GRAVITATIONAL WAVES (GW): PROBING the EARLYUNIVERSE (t . 1 s)
1 WEAKNESS of GRAVITY:
ADVANTAGE: GW DECOUPLE upon ProductionDISADVANTAGE: DIFFICULT DETECTION
2 ADVANTAGE: GW → Probe for Early Universe
→
Decouple→ Spectral Form RetainedSpecific HEP ⇔ Specific GW
3 Physical Processes:
InflationReheatingPhase TransitionsTurbulence
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GRAVITATIONAL WAVES (GW): PROBING the EARLYUNIVERSE (t . 1 s)
1 WEAKNESS of GRAVITY:
ADVANTAGE: GW DECOUPLE upon ProductionDISADVANTAGE: DIFFICULT DETECTION
2 ADVANTAGE: GW → Probe for Early Universe
→
Decouple→ Spectral Form RetainedSpecific HEP ⇔ Specific GW
3 Physical Processes:
InflationReheatingPhase TransitionsTurbulence
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GRAVITATIONAL WAVES (GW): PROBING the EARLYUNIVERSE (t . 1 s)
1 WEAKNESS of GRAVITY:
ADVANTAGE: GW DECOUPLE upon ProductionDISADVANTAGE: DIFFICULT DETECTION
2 ADVANTAGE: GW → Probe for Early Universe
→
Decouple→ Spectral Form RetainedSpecific HEP ⇔ Specific GW
3 Physical Processes:
InflationReheatingPhase TransitionsTurbulence
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PHYSICAL CONTEXT: REHEATING
INFLATION −→ REHEATING −→ BIG BANG THEORY
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PHYSICAL CONTEXT: REHEATING
INFLATION −→ REHEATING −→ BIG BANG THEORY
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PHYSICAL CONTEXT: REHEATING
INFLATION −→ REHEATING −→ BIG BANG THEORY
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PHYSICAL CONTEXT: REHEATING
INFLATION −→ REHEATING −→ BIG BANG THEORY
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PHYSICAL CONTEXT: REHEATING
INFLATION −→ REHEATING −→ BIG BANG THEORY
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SCALAR REHEATING: SIMPLE EXAMPLES
V (φ, χ) = 14λφ
4 + 12m
2χχ
2 + 12g
2φ2χ2 (Chaotic)
V (φ, χ) = 12µ
2φ2 + λ4 (χ2 − v2)2 + 1
2g2φ2χ2 (Hybrid)
φ(t) + 3Hφ+ V ′(φ) = 0 (Inflaton Zero Mode : Damped Oscillator)
φk + F (∫dqφqχ|k−q|)φk + ... = 0 (Inflaton Fluctuations)
χk + F (∫dqχq, φ|k−q|)χk + ... = 0 (Matter Fluctuations)
DYNAMICS:
Non-Linear, Non-Perturbative and Far-From-Equilibrium
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Reheating (Hybrid Scenarios): SPINODAL INSTABILITY
φ(t) + (µ2 + g2|χ|2)φ(t) = 0
χk +(k2+ m2
(φ2
φ2c− 1)
+λ|χ|2)χk = 0
(k < m =
√λv)
χk, nk ∼ e√m2−k2t
Hybrid Preheating
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Scalar Reheating: Observable Phenomena
PHENOMENA FROM (SCALAR) REHEATING:
SUB-HORIZON GRAVITATIONAL WAVES
SUPER-HORIZON GRAVITATIONAL WAVES
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EXPECTATIONs of (p)REHEATING: SubH-GW
Physics of (p)REHEATING: ϕk + ω2(k, t)ϕk = 0
Hybrid Preheating : ω2 = k2 +m2(1− V t) < 0 (Tachyonic)
Chaotic Preheating : ω2 = k2 + Φ2(t) sin2 µt (Periodic)
At ki: ϕki, nki
∼ eµ(k,t)t ⇒ Inhomogeneities:
Li ∼ 1/ki
δρ/ρ & 1
v ≈ c
(p)REHEATING: VERY EFFECTIVE GW GENERATOR
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EXPECTATIONs of (p)REHEATING: SubH-GW
Physics of (p)REHEATING: ϕk + ω2(k, t)ϕk = 0
Hybrid Preheating : ω2 = k2 +m2(1− V t) < 0 (Tachyonic)
Chaotic Preheating : ω2 = k2 + Φ2(t) sin2 µt (Periodic)
At ki: ϕki, nki
∼ eµ(k,t)t ⇒ Inhomogeneities:
Li ∼ 1/ki
δρ/ρ & 1
v ≈ c
(p)REHEATING: VERY EFFECTIVE GW GENERATOR
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EXPECTATIONs of (p)REHEATING: SubH-GW
At ki: ϕki, nki
∼ eµ(k,t)t ⇒ Inhomogeneities:
Li ∼ 1/kiδρ/ρ & 1
GW from RELATIVISTIC WAVES of MATTER
Ga-Bellido et al ’02 (Hybrid Scenario: λ ≈ 0.1, V EV = 10−3Mp)
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EXPECTATIONs of (p)REHEATING: SubH-GW
At ki: ϕki, nki
∼ eµ(k,t)t ⇒ Inhomogeneities:
Li ∼ 1/kiδρ/ρ & 1
GW from RELATIVISTIC WAVES of MATTER
Ga-Bellido et al ’02 (Hybrid Scenario: λ ≈ 0.1, V EV = 10−3Mp)
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Lattice Simulations: Dynamics
• Scalars (nk 1): φ+ V,φ = 0, χa + V,χa = 0
Semi-classical regime πk ≈ κφk + ... (Squeezed States)
• FRW: H2 = 8πG3 ρ, a
a = − 4πG3 (ρ+ 3p) ,
ρ = 〈ρφ + ρχ + ...〉p = 〈pφ + pχ + ...〉
• GW: h′′ij + 2Hh′ij −∇2hij = 16πGΠTTij , Πij = Tij − 〈Tij〉FRW
ds2 = a2(−dη2 + (δij + hij)dxidxj), TT :hii = 0hij ,j = 0
TT dof carry energy out of the source!!!
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Lattice Simulations: Dynamics
• Scalars (nk 1): φ+ V,φ = 0, χa + V,χa = 0
Semi-classical regime πk ≈ κφk + ... (Squeezed States)
• FRW: H2 = 8πG3 ρ, a
a = − 4πG3 (ρ+ 3p) ,
ρ = 〈ρφ + ρχ + ...〉p = 〈pφ + pχ + ...〉
• GW: h′′ij + 2Hh′ij −∇2hij = 16πGΠTTij , Πij = Tij − 〈Tij〉FRW
ds2 = a2(−dη2 + (δij + hij)dxidxj), TT :hii = 0hij ,j = 0
TT dof carry energy out of the source!!!
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Lattice Simulations: Dynamics
• Scalars (nk 1): φ+ V,φ = 0, χa + V,χa= 0
Semi-classical regime πk ≈ κφk + ... (Squeezed States)
• FRW: H2 = 8πG3 ρ, a
a = − 4πG3 (ρ+ 3p) ,
ρ = 〈ρφ + ρχ + ...〉p = 〈pφ + pχ + ...〉
• GW: h′′ij + 2Hh′ij −∇2hij = 16πGΠTTij , ΠTT
ij = ∂iχa∂jχaTT
ds2 = a2(−dη2 + (δij + hij)dxidxj), TT :hii = 0hij ,j = 0
TT dof carry energy out of the source!!!
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Hybrid (p)Reheating (Part I)
g2 = 2λ = 0.25, v = 10−3Mp, VI = 0.024
Bubble Nucleation and Collisions (Animation by Alfonso Sastre)
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Hybrid (p)Reheating (Part I)
g2 = 2λ = 0.25, v = 10−3Mp, VI = 0.024
Bubble Nucleation and Collisions (Animation by Alfonso Sastre)
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Hybrid (p)Reheating (Part I)
g2 = 2λ = 0.25, v = 10−3Mp, VI = 0.024
Bubble Nucleation and Collisions (Animation by Alfonso Sastre)
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Hybrid (p)Reheating (Part I)
g2 = 2λ = 0.25, v = 10−3Mp, VI = 0.024
Bubble Nucleation and Collisions (Animation by Alfonso Sastre)
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Hybrid (p)Reheating (Part I)
g2 = 2λ = 0.25, v = 10−3Mp, VI = 0.024
Bubble Nucleation and Collisions (Animation by Alfonso Sastre)
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Hybrid (p)Reheating (Part I)
g2 = 2λ = 0.25, v = 10−3Mp, VI = 0.024
Bubble Nucleation and Collisions (Animation by Alfonso Sastre)
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Hybrid (p)Reheating (Part I)
g2 = 2λ = 0.25, v = 10−3Mp, VI = 0.024
Bubble Nucleation and Collisions (Animation by Alfonso Sastre)
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Hybrid (p)Reheating (Part I)
g2 = 2λ = 0.25, v = 10−3Mp, VI = 0.024
Bubble Nucleation and Collisions (Animation by Alfonso Sastre)
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Hybrid (p)Reheating (Part I)
g2 = 2λ = 0.25, v = 10−3Mp, VI = 0.024
Bubble Nucleation and Collisions (Animation by Alfonso Sastre)
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Hybrid (p)Reheating (Part I)
g2 = 2λ = 0.25, v = 10−3Mp, VI = 0.024
Bubble Nucleation and Collisions (Animation by Alfonso Sastre)
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Hybrid (p)Reheating (Part I)
g2 = 2λ = 0.25, v = 10−3Mp, VI = 0.024
Bubble Nucleation and Collisions (Animation by Alfonso Sastre)
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Hybrid (p)Reheating (Part I)
g2 = 2λ = 0.25, v = 10−3Mp, VI = 0.024
Bubble Nucleation and Collisions (Animation by Alfonso Sastre)
![Page 32: GRAVITATIONALWAVES FROM/AFTER REHEATINGbenasque.org/2010cosmology/talks_contr/176_Figueroa_Benasque2… · 2 ADVANTAGE: GW !Probe for Early Universe! ˆ Decouple !Spectral Form Retained](https://reader033.fdocuments.us/reader033/viewer/2022042909/5f3af2689a63780da87f5b24/html5/thumbnails/32.jpg)
Hybrid (p)Reheating (Part I)
g2 = 2λ = 0.25, v = 10−3Mp, VI = 0.024
Bubble Nucleation and Collisions (Animation by Alfonso Sastre)
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Hybrid (p)Reheating (Part I)
g2 = 2λ = 0.25, v = 10−3Mp, VI = 0.024
Bubble Nucleation and Collisions (Animation by Alfonso Sastre)
![Page 34: GRAVITATIONALWAVES FROM/AFTER REHEATINGbenasque.org/2010cosmology/talks_contr/176_Figueroa_Benasque2… · 2 ADVANTAGE: GW !Probe for Early Universe! ˆ Decouple !Spectral Form Retained](https://reader033.fdocuments.us/reader033/viewer/2022042909/5f3af2689a63780da87f5b24/html5/thumbnails/34.jpg)
Hybrid (p)Reheating (Part I)
g2 = 2λ = 0.25, v = 10−3Mp, VI = 0.024
Bubble Nucleation and Collisions (Animation by Alfonso Sastre)
![Page 35: GRAVITATIONALWAVES FROM/AFTER REHEATINGbenasque.org/2010cosmology/talks_contr/176_Figueroa_Benasque2… · 2 ADVANTAGE: GW !Probe for Early Universe! ˆ Decouple !Spectral Form Retained](https://reader033.fdocuments.us/reader033/viewer/2022042909/5f3af2689a63780da87f5b24/html5/thumbnails/35.jpg)
Hybrid (p)Reheating (Part II)
g2 = 2λ = 0.25, v = 10−3Mp, VI = 0.024
3 stages: Exp. Instabilities → Bubble Collisions → Turbulence
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Hybrid (p)Reheating (Part II)
g2 = 2λ = 0.25, v = 10−3Mp, VI = 0.024
3 stages: Exp. Instabilities → Bubble Collisions → Turbulence
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Today’s Signal (GW RedShifted)
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Scalar Reheating: Observable Phenomena
PHENOMENA FROM (SCALAR) REHEATING:
SUB-HORIZON GRAVITATIONAL WAVES√
SUPER-HORIZON GRAVITATIONAL WAVES
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Hybrid Reheating = Phase Transition
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Hybrid Reheating = Phase Transition
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Hybrid Reheating = Phase Transition
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Hybrid Reheating = Phase Transition
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Aftermath of Hybrid Reheating: NLSM → GW
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Aftermath of Hybrid Reheating: NLSM → GW
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Aftermath of Hybrid Reheating: NLSM → GW
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Aftermath of Hybrid Reheating: NLSM → GW
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Aftermath of Hybrid Reheating: Scale Inv SubH GW
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Summary: GW from Scalar (p)Reheating
1 GW are Early Universe Ideal Probe: decoupled upon production ⇒spectral signature retained till today ⇒ GWB: “photo“ of very EarlyUniverse
2 GW from Reheating: Form, freq. Peak and Amplitude→ Specific Model of Inflation (Disadvantage/Advantage)
3 Scalar Reheating Models: GW (high amplitude, too high frequency)
4 Hybrid Reheating Models: GW (high amplitude, within BBO)
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Summary: GW from Scalar (p)Reheating
1 GW are Early Universe Ideal Probe: decoupled upon production ⇒spectral signature retained till today ⇒ GWB: “photo“ of very EarlyUniverse
2 GW from Reheating: Form, freq. Peak and Amplitude→ Specific Model of Inflation (Disadvantage/Advantage)
3 Scalar Reheating Models: GW (high amplitude, too high frequency)
4 Hybrid Reheating Models: GW (high amplitude, within BBO)
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Summary: GW from Scalar (p)Reheating
1 GW are Early Universe Ideal Probe: decoupled upon production ⇒spectral signature retained till today ⇒ GWB: “photo“ of very EarlyUniverse
2 GW from Reheating: Form, freq. Peak and Amplitude→ Specific Model of Inflation (Disadvantage/Advantage)
3 Scalar Reheating Models: GW (high amplitude, too high frequency)
4 Hybrid Reheating Models: GW (high amplitude, within BBO)
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Summary: GW from Scalar (p)Reheating
1 GW are Early Universe Ideal Probe: decoupled upon production ⇒spectral signature retained till today ⇒ GWB: “photo“ of very EarlyUniverse
2 GW from Reheating: Form, freq. Peak and Amplitude→ Specific Model of Inflation (Disadvantage/Advantage)
3 Scalar Reheating Models: GW (high amplitude, too high frequency)
4 Hybrid Reheating Models: GW (high amplitude, within BBO)
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Summary: Scale-Inv GW from Global PhT.
1 NLSM + large-N limit: Self-Ordering Scalar Fields after SSB(Global PhT).
2 kη∗ 1→ kη 1 : ΩGW (k, η) = const.Observable at LIGO, LISA, BBO,...
3 For V EV = MI , then ΩGW /ΩinfGW ∼ O(10)−O(100)
Scale-Inv GW is not any more a smoking gun of inflation.
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Summary: Scale-Inv GW from Global PhT.
1 NLSM + large-N limit: Self-Ordering Scalar Fields after SSB(Global PhT).
2 kη∗ 1→ kη 1 : ΩGW (k, η) = const.Observable at LIGO, LISA, BBO,...
3 For V EV = MI , then ΩGW /ΩinfGW ∼ O(10)−O(100)
Scale-Inv GW is not any more a smoking gun of inflation.
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Summary: Scale-Inv GW from Global PhT.
1 NLSM + large-N limit: Self-Ordering Scalar Fields after SSB(Global PhT).
2 kη∗ 1→ kη 1 : ΩGW (k, η) = const.Observable at LIGO, LISA, BBO,...
3 For V EV = MI , then ΩGW /ΩinfGW ∼ O(10)−O(100)
Scale-Inv GW is not any more a smoking gun of inflation.
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Back Slides
BACK SLIDES
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Aftermath Hybrid Reheating: Matter Perturbations
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Aftermath Hybrid Reheating: Matter Perturbations
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Aftermath Hybrid Reheating: Matter Perturbations
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Aftermath Hybrid Reheating: Matter Perturbations
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Aftermath Hybrid Reheating: Non-Gaussianity
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Aftermath Hybrid Reheating: Non-Gaussianity
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Aftermath Hybrid Reheating: Non-Gaussianity
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Aftermath Hybrid Reheating: Non-Gaussianity
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Aftermath Hybrid Reheating: Non-Gaussianity
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Aftermath Hybrid Reheating: Non-Gaussianity
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Aftermath Hybrid Reheating: Non-Gaussianity
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Aftermath Hybrid Reheating: Non-Gaussianity
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Aftermath Hybrid Reheating: Non-Gaussianity
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Aftermath Hybrid Reheating: Non-Gaussianity
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Aftermath Hybrid Reheating: Non-Gaussianity
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Back Slides
Turbulence
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Results for Hybrid Reheating: Turbulence
Turbulece: var(φ) ∼ t−2p, n(k, t) = t−γpno(t−pk) (M,T ’04)
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Results for Hybrid Reheating: Turbulence
Turbulece: var(φ) ∼ t−2p, n(k, t) = t−γpno(t−pk) (M,T ’04)
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Results for Hybrid Reheating: Turbulence
Turbulece: var(φ) ∼ t−2p, n(k, t) = t−γpno(t−pk) (M,T ’04)
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Back Slides
Lattice Techniques
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Lattice Simulations: Numerics
∂µO(x)→ (O(x+ µ)−O(x− µ))/2aµ
∂µ∂µO(x)→ (O(x+ 2µ) +O(x− 2µ)− 2O(x))/4a2µ
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GW extraction
Scalar Source (Configuration Space):
hij(x, t) + 3Hhij(x, t)− 1a2∇2hij(x, t) = 16π
a2 TT ∇lφa∇mφa (x, t)
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GW extraction
Scalar Source (Configuration Space):
hij(x, t) + 3Hhij(x, t)− 1a2∇2hij(x, t) = 16π
a2 TT ∇lφa∇mφa (x, t)
Scalar Source (Fourier):
hij(k, t) + 3Hhij(k, t) + k2
a2 hij(k, t) = 16π Λij,lm(k) ∇lφa∇mφa (k, t)
Λij,lm = PilPjm − 12PijPlm, Pij = δij − kikj/k2
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GW extraction
Scalar Source (Configuration Space):
hij(x, t) + 3Hhij(x, t)− 1a2∇2hij(x, t) = 16π
a2 TT ∇lφa∇mφa (x, t)
Scalar Source (Fourier):
hij(k, t) + 3Hhij(k, t) + k2
a2 hij(k, t) = 16π Λij,lm(k) ∇lφa∇mφa (k, t)
Λij,lm = PilPjm − 12PijPlm, Pij = δij − kikj/k2
Solution: (hij(t0) = hij(t0) = 0)
hij(k, t) = Λij,lm(k)∫ tt0dt′G(t− t′)Πeff
lm(k, t′), Πefflm = ∇lφ∇mφ
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GW extraction (II)
Building the Solution:
1) Non-Physical eq.:
uij(x, t) + 3Huij(x, t)− ∇2
a2 uij(x, t) = 16π φa,i φa,j (x, t)
2) Fourier transform: uij(x, t)→ uij(k, t)
3) Proyection: hij(k, t) = Λij,lm(k)ulm(k, t)
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GW extraction (II)
Outputs: ρGW = 132πG
1L3
∫d3x hij hij = 1
32πG1L3
∫d3k|hij(t,k)|2
1) Total GW density:ρGW = 1
32πGL3 ×∫k2dk
∫dΩ Λij,lm(k)uij(t,k)u∗lm(t,k)
2) Spectrum: dρd log k = 1
8GL3 k3⟨
Λij,lm(k)uij(t,k)u∗lm(t,k)⟩
4π
3) Snapshots: hij(t,x) = (2π)−3/2∫d3ke−ikxΛij,lm(k)ulm(t,k)