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We introduce the eikonal approximation to study the effect of the large-scale motion of cosmic fluids on their small-scale evolution.
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Another case studied in PT with two components following geodesic motion is a mixture of CDM and clustering quintessence [ 23 ] . However, in this case the initial conditions are such that the two fluids remain comoving during their evolution and isodensity modes do not develop
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It is straightforward to show that for Λ \Lambda CDM f − = − 3 2 Ω m f_{-}=-\frac{3}{2}\Omega_{m} and f + / f − = 1 − 5 3 a D + f_{+}/f_{-}=1-\frac{5}{3}\frac{a}{D_{+}}
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In this paper we will indistinguishably use the term of propagator for both ξ a b \xi_{ab} and G a b G_{ab} although the latter is the ensemble average of the former
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We are here in a situation comparable to that encountered in Lagrangian space where the displacement is found to be non-potential at order three and beyond in PT
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Note that contrary to the notation of [ 21 ] , here θ \theta denotes the dimensionless
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