The development of gravitational instabilities - RESCEU

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Changing gravity There are many ways of doing so... (Jain, Zhang PRD ’08) 1 H ˙θ(k) + (2 + If the change is such that Ḣ H 2 )θ(k)+3 2 Ω m ξ(k, t) δ m (k) =... f k ≡ d log D + d log a = Ω ( m γ γ GR ≈ 0.55 ) standard parameterization (Amendola & Quercellini, ’04, Linder ’05, Reyes et al. Nature, etc.), 4.87 FB, Brax (in prep) S3⩵3Ν2 4.86 4.85 This is still a modest change 4.84 GR ‘‘DGP’’ 0.5 0.55 0.6 0.65 0.7 0.75 0.8 Γ
In presence of a dilaton field Brax et al. astro-ph/1005.3735 S = ∫ d 4 x √ { } M 2 ∫ −g Pl 2 R − M Plg 2 µν k 2 (φ)∂ µ φ∂ ν φ − V (φ) + This extra field φ that is responsible of massive gravity effects. Its effect are suppressed in dense regions through the Chameleon mechanism. A(φ) = 1 + A 2 2 (φ − φ 0) 2 + . . . A new force term: F i = − 1 a(t) V (φ) =A 4 (φ)V 0 exp(−φ) ( ) 2 d log A k 2 (φ) =3 + 1 dφ λ 2 d 4 x √ −˜gL m (ψ (i) m ,A 2 (φ)g µν ) , ( Φ(x,t) ,i + d log A dφ ( ¯φ + δφ)φ(x,t) ,i ) An effective potential for the dilaton field Newton potentials, with standard Poisson equation V eff. (φ) =A 4 (φ)V 0 exp(−φ)+A(φ)ρ m
Page 1: Francis Bernardeau IPhT Saclay, Fra
Page 4 and 5: Which observables ? 〈δ x (k 1 )
Page 6 and 7: A self-gravitating expanding dust f
Page 8 and 9: ‣Motion equations in Fourier spac
Page 10 and 11: ‣ A lot is known at tree order Th
Page 12 and 13: A field theory reformulation Scocci
Page 14 and 15: Not a standard quantum field theory
Page 16: The closure theory Valageas P., A&A
Page 19 and 20: One key ingredient : the propagator
Page 21 and 22: ‣ RPT (Scoccimarro and Crocce) co
Page 23 and 24: Insights into higher order propagat
Page 25 and 26: ‣ This suggests another scheme :
Page 27 and 28: Comparison with numerical simulatio
Page 29 and 30: • Does it speed up the convergenc
Page 31: Using large-scale structure to test
Page 35 and 36: Evolution of structure: from GR to
Page 37 and 38: Bispectra (equilateral configuratio

The development of gravitational instabilities - RESCEU

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