Cosmological Perturbations and Structure Formation via STOCHASTIC GRAVITY B. L. Hu University of Maryland KITP- UCSB Conference on Nonequilibirum Phenomena in Cosmology and Particle Physics (Feb 25-29, 2008) Reporting on work of Roura and Verdaguer. slides courtesy E. Verdaguer OUTLINE 1. Semiclassical gravity (SCG): SC Einstein Eqn: <Tmn> 2. Stochastic gravity: Einstein-Langevin Equation Noise Kernel: <Tmn Trs> 3. Influence functional; Stochastic Effective Action. 4. One area of Application: Primordial cosmological perturbations • Gives result equivalent at linear order to usual method of quantizing metric and inflaton perturbations • But can treat quadratic order perturbations needed in R2 e.g., trace anomaly driven (Starobinsky) inflation . SEMICLASSICAL GRAVITY Semiclassical Einstein eq. for classical geometry, metric function g ˆ 2 Ggab[]= κ〈〉 Tgab [] ren κπ==88/Gm πP Klein-Gordon eq. for quantum matter field ^φ 22 ˆ ()0∇g −−mRξφ = • Solve for g and ^φ self-consistently. • Backreaction problem is at the heart of semiclassical gravity. SEMICLASSICAL EINSTEIN EQUATION Renormalization introduces quadratic tensors ˆ Ggab[]+Λ gab −αβκ Ag ab [] − Bgab [] = 〈 Tgab [] 〉 ren where 1 δ Aab =−dx4 gC Ccdef ∫ cdef −g δ gab 1 δ Bab =−∫ dx42 gR −g δ gab 1 TgmgGab=∇ aφ ∇ bφφφφξ −ab()() ∇ c ∇ +22 +ab ∇∇ c −∇ a ∇ b + ab φ2 2 cc LIMITS OF SEMICLASSICAL GRAVITY • Below Planck energy: measurements of time and length intervals Δtt, >> P Δl>> lP • Quantum fluctuations of stress tensor small: 〈TTˆˆ22〉−〈 〉 ≈0 We want to extend semiclassical Einstein equations to ˆ account for fluctuations ofTab consistently. Semiclassical Gravity Semiclassical Einstein Equation (schematically): + κ (Tμν) c is the Einstein tensor (plus covariant terms associated with the renormalization of the quantum field) Free massive scalar field Stochastic Gravity Einstein- Langevin Equation (schematically): How could a quantum field give rise to a stochastic source? via Influence functional (Feynman-Vernon 1963): • We will assume linear perturbation of semiclassical solution ghab+ ab But stochastic gravity is NOT restricted to linear perturbations ˆ • Einstein-Langevin equation: GTgh++=〈〉+κξ()gh (1) ˆ (1) Gab []g +=〈hTκκab []g +〉+h renξ ab []g 22 ˆ ()0∇−gh+ mR −ξφ = NOISE KERNEL • Exp Value of 2-point correlations of stress tensor: bitensor • Noise kernel measures quantum flucts of stress tensor 1 Nxytxty(, )=〈ˆˆ (),( )} 〉 tTˆ ≡ ˆˆˆ−〈 TI 〉 abcd 2 { ab cd ab ab ab It can be represented by (shown via influence functional to be equivalent to) a classical stochastic tensor source ξab[]g 〈〉=ξab s 0 〈ξab()x ξ cd ()yNxy〉= s abcd (, ) • Symmetric, traceless (for conformal field), divergenceless Noise associated with the fluctuations of a quantum field • The noise kernel is real and positive semi-definite as a consequence of stress energy tensor being self-adjoint • Classical Gaussian stochastic tensor field: denotes statistical average wrt this noise distribution Classical Stochastic Field assoc.with a Quantum Field • Stochastic tensor is covariantly conserved in the background spacetime (which is a solution of the semiclassical Einstein equation). • For a conformal field is traceless: Thus there is no stochastic correction to the trace anomaly INFLUENCE FUNCTIONAL • Open quantum system (Feynman-Vernon 63) system environment hab φ j Fe≡=iSIF Dφφ Dexp( S⎡⎤⎡⎤ φ , g+−− S φ,) g IF ∫ [ +−] [ ] m ⎣⎦⎣⎦ +m − ± 1 ˆ i SghIF ()+=〈〉− Thx[] x [] hHhx xy{} y +[] hNhx xy⎡ y ⎤ 28∫∫∫∫∫⎣ ⎦ + − +− (x,y denotes ab.cd) []hhh≡ − {hhh} ≡+()/2 1 i H '*= Im〈〉−〈〉TTT (ˆˆ )⎡ TT ˆ , ˆ⎤ xy 48x y ⎣ x y ⎦ 〈+〉=−−Tgh(1)[] 2 dygHxyhy4 (,)()cd ab ren ∫ abcd INFLUENCE FUNCTIONAL •Closed Time Path effective action at tree level in metric pert. (0) ⎡⎤⎡⎤⎡⎤⎡⎤+− + − +− 3 Γ=−++CTP⎣⎦⎣⎦⎣⎦⎣⎦hh,, Sh ggI Sh SF hh Oh( ) Sg is EH action plus quadratic terms. • Integral identity (Feynman Vernon 1963): ⎛⎞⎛11i ⎞ −Im SIF ⎡⎤ −1 eexp≡−⎜⎟⎜[]hNxxyy⎣⎦ h∝ Dξξξξexp −xxyyN + zz[] h ⎟ ⎝⎠⎝82∫∫ ∫ ∫∫2 ∫ ⎠ • Probability distribution functional of a 1 −1 − ∫∫ξ N ξ Pe[]ξ ∝ 2 classical stochastic field ξab ()x ⎛⎞⎛⎞11 +− iS⎜⎟⎜⎟ReIF ++∫∫ξξ [ h ] iS ReIF [ h ] eDPeeiSIF [,] h h =≡∫ ξξ[]⎝⎠⎝⎠22 s STOCHASTIC EFFECTIVE ACTION • Define a stochastic effective action: +− + − 1 Γ=−++⎡⎤⎡⎤⎡⎤hh,;ξξ S h S hRe S[] h stc ⎣⎦⎣⎦⎣⎦g g IF 2 ∫ z z • field equation from: δΓstc + = 0 δ h hh± = the Einstein-Langevin equation (1) ˆ (1) Gghab []+=〈κκ Tghab [] +〉+renξ ab [] g SOLUTIONS OF EINSTEIN-LANGEVIN EQUATIONS • These stochastic equations determine the correlations hx()=+ hx04 ()κξ dx ' −gGxxxret (, ')cd (') ab ab ∫ abcd 〈〉=〈〉+hxhy() () hxhy00 () () κ 2 Gret (, xxN ')efgh (',') xyGret ( yy ',) ab cd s ab cd s ∫∫ abef ghcd Intrinsic fluctuations + Induced fluctuations (flucts in the initial state) (due to matter field flucts) • Stochastic metric correlations is equivalent to quantum metric correlations in 1/N: (Calzetta, Roura, Verdaguer) 1 〈 hxhyˆˆ(), ()〉=〈 hxhy () () 〉 2 { ab cd } ab cd s Roura Hu (06, 07) Roura & Verdaguer (99, 07), Urakawa and Maeda (07) Hu 03 STOCHASTIC GRAVITY AND PRIMORDIAL COSMOLOGICAL PERTURBATIONS • Quantum fluctuations of inflaton are seeds for structure formation • Simplest chaotic inflationary model (Linde): Massive minimally coupled inflaton field, initially at average value larger than Planck scale V ()φ 2 << <~ φ φ& V ()φ mP φ0 11 Lm()φ =∂∂+φφa 22 φ 22a • Background inflaton field and FRW metric ˆ 22 2 ij φ()ηφ=〈 〉 ds=−+ a()(ηηδ dij dx dx ) PERTURBATIONS • Inflaton and scalar metric perturbations ˆ φφηϕ()xx=+ ()ˆ () 〈ϕˆ〉=g 0 22 2 ij ds=−+Φ+−Ψ a ()[(12ηηδ )d (12 )ij dx dx ] • Einstein-Langevin equations (0) ˆˆ(0) (1) (1) Ggab []−〈κκκ Tgab [] 〉+ Ghab [] −〈 Thab [] 〉=ξab [] g zeroth order metric g is assumed to be quasi- de Sitter. ˆ ˆˆ1 ˆˆc 22 ˆ Tgmab=∇%% aφ ∇ bφφφφ −% ab() ∇ %% c ∇ + ggh% = + 2 1 ˆˆ tTˆ ≡−〈〉ˆˆ T 〈〉=〈〉ξξ()()xys {}tx (),() tyg [] 2 STRESS TENSOR CORRELATIONS ˆˆ ˆ ˆ 〈+〉=〈+〉+〈+〉+〈+〉Tg[] h Tg [] hφφφ Tg [] hϕϕ Tg [] h ϕ 〈〉=〈〉+〈〉≡〈〉+〈〉ttˆˆ,[] g tt ˆˆ ,[] g tt ˆˆ ,[] g ξξ(1)(1) ξξ (2)(2) {} {} φϕ22 { } ϕϕ22 s s • assume Gaussian state: 〈ϕˆ〉=0 〈ϕˆˆˆϕϕ〉=0 • two independent stochastic sources: ξ (1),ξ (2) independently conserved • Including only the first (linear) term: 〈···〉 φ 22ϕ we will show that the stochastic gravity formulation gives equivalent results as the traditional quantized metric and scalar field perturbations E-L eqn for linear perturbations ˆ ξ = 0,(ij≠ ) •Since 〈〉=Tiij 0,( ≠j ) ij metric perturbations Φ =Ψ • Fourier transf. of 0i-component: (neglecting non-local term): a '(η ) 2(kHikkΦ+Φ ') =κξ ki(0 ) H ≡ a()η • Retarded propagator for Φk k κη⎛⎞a() Gfret (,η ηθηηηη ')=−+⎜⎟ ( ') (, ') 2('kai ⎝⎠η ) With we get for the ii component of E-L eqn: Two unknowns 1. 2. These three equations reduce to two because of the Bianchi Identity, which holds here since the averaged and stochastic sources in the EL eqn are separately conserved. Equivalence with Quantum approach: Can show that EL eqn reduces to (Roura and Verdaguer 2007) Same as the conventional approach via quantized linear perturbations, e.g., Eq. (6.48) of Comments: 1. In Fourier space nonlocal terms in the integro-differential equation in the spatial sector simplify to products. Non-locality in time in this equation disappears due to an exact cancellation of the different contributions from 2. Seems like there is no dependence on the stochastic source. But the solutions to ELeqn should also satisfy the constraint eqn at the initial time in addition to the dynamical eqn. The initial conditions for have dependence on the stochastic source. CORRELATIONS FOR METRIC PERTURBATIONS • Solutions of E-L equation: r r 〈Φ()ηη Φ (') 〉 = (2) πδ2' (kk + ') Gkk 〈 ξξ 〉 G k k'' s ∫∫ ret k k s ret 1 ˆˆ 〈〉≡〈〉ξξkk'' s{}tt k, k 2 ˆˆkk− 〈〉{tt010ii(),()η η 2} =〈 kk ii φηφη '()'()1 2{ ϕηˆˆk (),() 1 ϕ− k η 2} 〉 (1) 〈〉{ϕˆˆkk(),()ηϕη12− } =G k (, ηη 12 ) is the Hadamard function for free scalar field on de Sitter, in Euclidean vacuum 1 a()ηη= −−∞<< ; 0 Hη METRIC PERTURBATION CORRELATIONS (1) mm/ Computing Gk perturbatively in P ~ 2 assuming slow roll φ&()tmmm − P ( /P ) taking (rather insensitive to initial conds.) η0 →−∞ 2 233⎛⎞m − rr 〈Φkks()η Φ' (')ηπ 〉 8⎜⎟kkkk (2) πδ (+ ')cos[( ηη − ')] ⎝⎠mP • Harrison-Zel’dovich scale inv. spectrum large scales kη ≤1 m −6 • Amplitude of CMB anisotropies ~ 10 mP • Agreement with linear perturbations approach (Mukhanov 92) • Stochastic gravity can go beyond linear app. in inflaton flucts. (Weinberg 05) and deal with Starobinsky (tr anomaly) inflation Summary: Main Features 1. Semiclassical gravity depends on e.v. of q. stress tensor S.G fails when flucts. of quantum stress tensor are large 2. Stochastic gravity incorporates these fluctuations (at Gaussian level) through the noise kernel acting as source for the Einstein-Langevin equation 3. Stochastic two-point metric correlations agree with quantum two-point metric correlations to order 1/N in large N expansion 4. Cosmological Perturbation and Structure Formation: Agreement with linear perturbations approach (e.g.,Mukhanov 92) •But can go beyond linear order in inflaton fluctuations necessary for trace-anomaly driven inflations (e.g., Starobinsky 1980) Stochastic Gravity program • (since 1994) E. Calzetta (Buenos Aires), B. L. Hu, A. Matacz, N.G. Phillips, S. Sinha (Maryland) A. Campos, R. Martin, A. Roura, Enric Verdaguer (Barcelona); • Current work: with A. Roura (Los Alamos), Enric Verdaguer (Barcelona) - cosmological perturbations work // by Urakawa and Maeda (Waseda) • Review: B. L. Hu and E. Verdaguer, “Stochastic gravity: Theory and Applications”, in Living Reviews in Relativity 7 (2004) 3. [update