towards a ghost- and singularity-free theory of gravity · curvature is power-counting...
TRANSCRIPT
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Towards a ghost- and singularity-free
theory of gravity
Luca Buoninfante
International School of Subnuclear physics57° Course – Erice – Sicily
21-30 June 2019
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Introduction
• Einstein’s general relativity (GR) has been tested to veryhigh precision in the IR regime;
• Despite the great succes of GR, there are still openproblems that make the theory incomplete in the UVregime, e.g. Blackhole and Cosmological singularities,non-renormalizability [‘t hooft, Veltmann (1974); Goroff, Sagnotti (1985)]
• To what extent is GR valid in the UV?
• The inverse-square law of Newton’s potential has beentested only up to 5.6 × 10−5meters with torsion balanceexperiments.
𝑆 =1
16𝜋𝐺න𝑑4𝑥 −𝑔ℛ
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Introduction
Our knowledge of the gravitational interaction
at short distances is really limited!
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4th order gravity
• The 4th order gravitational action quadratic in the curvature is power-counting renormalizable:
𝑆 =1
16𝜋𝐺න𝑑4𝑥 −𝑔 ℛ + 𝛼ℛ2 + 𝛽ℛ𝜇𝜈ℛ
𝜇𝜈
• Unitarity is violated at the tree-level:
• Conflict: Unitarity VS Renormalizability!
Spin-2 ghost degree of freedom
[Stelle, 1977, PRD]
Π 𝑘 = Π𝐺𝑅 +1
2
𝒫0
𝑘2+𝑚02 −
𝒫2
𝑘2+𝑚22 ,
𝑚0 ≔ 3𝛼 +𝛽 −1/2
𝑚2 ≔ −1
2𝛽
−1/2
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Unitarity VS Renormalizability
• Einstein’s GR is unitary but non-renormalizable, while4th order quadratic gravity is power-countingrenormalizable but non-unitary!
Several (recent) attempts:
• Asymptotically safe gravity [Eichhorn’s and Schiffer’s talks…]
• 4th order gravity with Fakeons [Anselmi & Piva 2017+]
• Lee-Wick gravity theories [Modesto & Shapiro 2016+; Anselmi & Piva 2017+]
• Nonlocal gravity theories [Efimov, Krasnikov, Kuz’min, Tomboulis, Biswas, Mazumdar, Koshelev, Modesto, Rachwal….]
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• Local (polynomial) Lagrangians:
ℒ𝐿 ≡ ℒ𝐿 𝜙, 𝜕𝜙, 𝜕2𝜙,… , 𝜕𝑛𝜙
• Nonlocal (non-polynomial) Lagrangians:
ℒ𝑁𝐿 ≡ ℒ𝑁𝐿 𝜙, 𝜕𝜙, 𝜕2𝜙,… , 𝜕𝑛𝜙,… , 𝑒⧠𝜙, ln ⧠ 𝜙,1
⧠𝜙,…
Local VS Nonlocal
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• Finite order derivative theory:
ℒ𝐿 =1
2𝜙⧠ ⧠+𝑚2 𝜙 ⟹ Π𝐿(𝑝) =
1
𝑚2
1
𝑝2−
1
𝑝2 +𝑚2
• Infinite order derivative theory:
Π𝑁𝐿 𝑝 =𝐹 𝑝2
𝑝2 +𝑚2=
𝑛=0
∞
𝐹𝑛𝑝2𝑛
𝑝2 +𝑚2
• Is there any higher derivative operator 𝐹 𝑝2 such that the propagator is ghost-free? YES!
Local VS Nonlocal
GHOST!
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• Nonlocal scalar field:
ℒ =1
2𝜙𝑒−𝛾 ⧠/𝑀𝑠
2⧠+𝑚2 𝜙 + 𝑉 𝜙 ,
𝛾 ⧠/𝑀𝑠2 =
𝒏=𝟎
∞
𝛾𝒏⧠
𝑀𝑠2
𝒏
• Ghost-free propagator:
Π 𝑝 =𝑒−𝛾 −𝑝2/𝑀𝑠
2
𝑝2 +𝑚2
Renormalizability for some specific entire functions
[Modesto 2011; Modesto & Rachwal 2014]
Perturbative unitarity (optical theorem and Cutkosky rules)[Pius & Sen 2015; Briscese & Modesto 2018; Chin & Tomboulis 2018]
Causality violation at microscopic scales (acausal Green functions and local commutativity violation)[Tomboulis 2015; LB, Lambiase, Mazumdar 2018]
Exponential of entire functions
Entire function: No extra poles!
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Infinite Derivative Gravity (IDG)
• Non-local higher derivative theories can be ghost-free:
• Ghost-free propagator:
• Entire function, e.g.
[Kuz’min, 1989; Tomboulis 1997; Biswas et al., 2006,2011; Modesto et al. 2011+]
𝑒−𝛾 ⧠/𝑀𝑠2= 𝑒−⧠/𝑀𝑠
2
Π𝜇𝜈𝜌𝜎 𝑘 = 𝑒𝛾(−𝑘2/𝑀𝑠
2)Π𝜇𝜈𝜌𝜎𝐺𝑅 𝑘 = 𝑒𝛾(−𝑘
2/𝑀𝑠2)
𝒫𝜇𝜈𝜌𝜎2
𝑘2−𝒫𝜇𝜈𝜌𝜎0
2𝑘2
𝑆 =1
16𝜋𝐺න𝑑4𝑥 −𝑔 ℛ + 𝐺𝜇𝜈𝐹(⧠)ℛ
𝜇𝜈 , 𝐹 ⧠ =𝑒−𝛾 ⧠/𝑀𝑠
2− 1
⧠
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• Linearized metric for a static point-like source:
𝑑𝑠2 = − 1 + 2𝜙 𝑟 𝑑𝑡2 + 1 − 2𝜙 𝑟 (𝑑𝑟2 + 𝑟2𝑑Ω2)
[Tseytlin, 1995 PLB; Biswas et al., 2006 JCAP; Modesto, 2012 PRD; Biswas et al., 2012, PRL]
Singularity-free!
IR UV
𝑒−∇2
𝑀𝑠2∇2𝜙 Ԧ𝑟 = 4π𝐺𝑚𝛿(3) Ԧ𝑟 ⟹ 𝜙 𝑟 = −
𝐺𝑚
𝑟𝐸𝑟𝑓
𝑀𝑠𝑟
2
𝜙 𝑟 ~ −𝐺𝑚
𝑟𝜙 𝑟 ~−
𝐺𝑚𝑀𝑠
𝜋< ∞
𝐸𝑟𝑓 𝑥 ≔2
𝜋න0
𝑥
𝑒−𝑡2𝑑𝑡
Infinite Derivative Gravity (IDG)
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• Schwarzschild solution in Einstein’s GR:
• IDG case:
ℛ =𝐺𝑚𝑀𝑠
3𝑒−𝑀𝑠2𝑟2/4
𝜋
• Non-singular Kretschmann invariant!
• Smearing of the (delta-) source due to non-locality!
• The UV/short distances behavior is ameliorated!
“NON-VACUUM”SOLUTION!
[LB, et al. JCAP]
Infinite Derivative Gravity (IDG)
𝜙 𝑟 = −𝐺𝑚
𝑟⟹ ℛ𝐺𝑅 = 8𝜋𝐺𝑚𝛿(3) Ԧ𝑟
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• Linearized metric for a rotating ring source in IDG:
• Stress-energy tensor:
• Differential equations:
[LB, et al. PRD]
Infinite Derivative Gravity (IDG)
𝑑𝑠2 = − 1 + 2𝜙 𝑟 𝑑𝑡2 + 2ℎ ∙ 𝑑 Ԧ𝑟𝑑𝑡 + 1 − 2𝜙 𝑟 (𝑑𝑟2 + 𝑟2𝑑Ω2)
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• Linearized metric for a rotating ring source in IDG:
• Non-singular solutions:
[LB, et al. PRD]
Infinite Derivative Gravity (IDG)
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Summary and Outlook
• Non-local higher derivative Lagrangians can be ghost-free.
• Nonlocality can improve the high-energy/short-distance behavior.
• In the linear regime the spacetime metrics can be made non-singularin IDG: non-local gravitational interaction smears out the delta-source.
Open Problems
• Quantification of the causality violation?
• UV behavior of the tree-level amplitudes in nonlocal gravity?
• Huge arbitrarity on the choice of the entire function?
• Non-linear (non-singular) spacetime metric solutions?
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Thank you
for
your attention!
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• Nonlocal action:
𝑆 = න𝑑4𝑥𝑑4𝑦𝜙 𝑥 𝐾 𝑥 − 𝑦 𝜙 𝑦
= න𝑑4𝑥𝑑4𝑦𝜙 𝑥 න𝑑4𝑘
2𝜋 4𝐹 −𝑘2 𝑒𝑖𝑘∙ 𝑥−𝑦 𝜙 𝑦
= න𝑑4𝑥𝑑4𝑦 𝜙 𝑥 𝐹 ⧠ න𝑑4𝑘
2𝜋 4𝑒𝑖𝑘∙ 𝑥−𝑦 𝜙 𝑦
= න𝑑4𝑥𝑑4𝑦 𝜙 𝑥 𝐹 ⧠ 𝜙 𝑥
Extra Slides: nonlocality
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• NO time-ordered propagator:
𝑒−𝛾 ⧠ ⧠− 𝑚2 Π 𝑥 = 𝑖𝛿 4 𝑥 ,
Π 𝑥 = Π𝑐 𝑥 + Π𝑛𝑐 𝑥 , Π𝑛𝑐 𝑥 = 𝑖
𝑞=1
∞𝑖𝑞−1
𝑞!𝜕𝑥0(𝑞−1)
[𝑊 𝑞 𝑥 −𝑊 𝑞 −𝑥 ]
𝑊 𝑞 𝑥 = න𝑑4𝑘
2𝜋 4 𝑒𝑖𝑘∙𝑥𝜃(𝑘0)𝛿(𝑘2 +𝑚2)
𝜕(𝑞)𝑒−𝛾 −𝑘2
𝜕𝑘0(𝑞)
Extra slides: causality violation
[LB, Lambiase, Mazumdar, NPB]
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Extra slides: causality violation
• Acausal Green function:
𝑒−⧠𝑀𝑠2
2𝑛
⧠− 𝑚2 𝐺𝑅(𝑥 − 𝑦) = 𝑖𝛿 4 𝑥 − 𝑦 ,
[LB, Lambiase, Mazumdar, NPB]
𝐺𝑅 𝑥 − 𝑦 ≠ 0, 𝑓𝑜𝑟 (𝑥 − 𝑦)2 > 0
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Extra slides: unitarity
• Optical theorem:
• Ghost and unitarity violation:
• Nonlocal propagator:
𝑆+𝑆 = 1, 𝑆 = 1 + 𝑖𝑇 ⟹ 2𝐼𝑚 𝑇 = 𝑇+𝑇 > 0
𝑆+𝑆 = 1, 𝐼𝑚−1
𝑝2 − 𝑖𝜖= −
𝜖
𝑝2 + 𝜖2= −π𝛿 4 𝑝2 < 0
𝐼𝑚𝑒−𝑝
2/𝑀𝑠2
𝑝2 − 𝑖𝜖=𝑒−𝑝
2/𝑀𝑠2𝜖
𝑝2 + 𝜖2= π𝛿 4 𝑝2 > 0
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• Locality, causality, unitarity , renormalizability… too manyrequirements?
• Beyond higher order derivatives? Diffeomorphism invarianceallows more…
• General quadratic gravitational action, parity-invariant and torsion-free:
Extra slides: most general quadratic action
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• Analytic form-factors:
• Propagator:
• Ghost-free condition:
• Exponential of an entire function: NO extra poles!
[Tomboulis 1997; Modesto, 2012 PRD; Biswas et al., 2012, PRL]
Extra slides: ghost-free propagator
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Extra slides: spin projection operators
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• Tomboulis’ entire function:
𝛾 𝑧 = Γ 0, 𝑃 𝑧 + 𝛾𝐸 + 𝑙𝑜𝑔 𝑃 𝑧
• UV behavior:
z → ∞ ⟹ 𝑒𝛾 𝑧 ⟶ 𝑒𝛾𝐸𝑃 𝑧
Extra Slides: Renormalizable nonlocal gravity
[Tomboulis 1977]
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• All curvature invariants are singularity-free at r=0!
• Kretschmann invariant:
Extra slides: Non-singular curvature invariants
[LB, Koshelev, Lambiase, Mazumdar, JCAP. , LB, Koshelev, Lambiase, Marto, Mazumdar, JCAP]
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• Linearized metric for a rotating ring source in IDG:
• Solutions:
[LB, et al. PRD]
Extra slides: metric for rotating ring
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• Linearized metric for a rotating ring source in IDG:
• Non-singular solutions:
[LB, et al. PRD]
Extra slides: metric for rotating ring
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Multipole expansion in IDG
[L.B., et al., PRD]
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Introduction
Our knowledge of the gravitational interaction
at short distances is really limited!
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• Gravitational force/acceleration:
Extra slides: gravitational force
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• Linearized metric for a static charged point-like source in IDG:
[LB, Harmsen, Maheswari, Mazumdar, 1804.09624]
Singularity-free!
IR UV
Extra slides: metric for an electric charge
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• Trace of the field equations:
[Biswas, Conroy, Koshelev, Mazumdar, 2013, CQG]
Extra slides: trace eqution of IDG
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Extra slides: most general ghost-free choice for a(k) and c(k)
Exponentials of entire functions!
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Extra slides: non-local scale
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• Fourth order order gravity has curvature singularity:
• Theories with derivatives of order higher than 4 are singularity-free and conformally-flat at the origin:
Extra slides: Local vs Non-local
[Giacchini, Paula Netto, EPJC]
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• Non-local higher derivative theories can be made ghost-free at the tree-level.
• Is the Schwarzschild metric a solution of the full non-lineartheory?
Extra slides: Local vs Non-local
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• Is the Schwarzschild metric a solution of the full non-lineartheory?
• Non-local theories:
• Example of non-point support:
[L.B, Koshelev, Lambiase, Marto, Mazumdar, JCAP (2018)]
Extra slides: Local vs Non-local
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• Is the Schwarzschild metric a solution of the full non-lineartheory?
• Local theories: point-support!
• Non-local theories:
[L.B, Koshelev, Lambiase, Marto, Mazumdar, JCAP (2018)]
Non-point-support
Extra slides: Local vs Non-local
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• Schwarzschild metric as a solution coupled to a non-delta source distribution?
Hint from the linear regime
• In local theorie YES:
• In non-local theories (a-priori) NO:
Extra slides: Local vs Non-local
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• Stress-energy tensor for Schwarzschild metric in Kerr-Schild coordinates:
• Stress-energy tensor for Kerr metric in Kerr-Schild coordinates:
[H. Balasin, H. Nachbagauer, PLB 1993; CQG 1993.]
Extra slides: sources for Schwarzschild and Kerr metrics
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Extra slides: different nonlocal models
• P-adic string: [Freund, Witten, Frampton…1987+]
• Infinite Derivative Theories: [Krasnikov, Biswas, Mazumdar, Modesto…]
• Nonlocal model with complex conjugate poles: [LB, Lambiase, Yamaguchi 2018]
ℒ𝑝−𝑎𝑑𝑖𝑐 = −𝑚𝑠4
2𝑔𝑠2
𝑝2
𝑝 − 1𝜙𝑝
−⧠𝑚𝑠2𝜙, Π𝑝−𝑎𝑑𝑖𝑐 𝑘 = 𝑝
−𝑘2
𝑚𝑠2= 𝑒
−ln(𝑝)𝑘2
𝑚𝑠2
ℒ𝐼𝐷𝑇 =1
2𝜙𝑒−⧠/𝑀𝑠
2⧠𝜙, Π𝐼𝐷𝑇 𝑘 =
𝑒−𝑘2/𝑀𝑠
2
𝑘2
ℒ = −𝑀𝑠2
2𝜙(𝑒−⧠/𝑀𝑠
2− 1)𝜙, Π 𝑘 =
1
𝑀𝑠2(𝑒𝑘
2/𝑀𝑠2− 1)