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Unformatted text preview: Homework 3 William D. Linch III March 11, 2005 1.a The rate of change of a vector v a flowing along the integral curves of u a is given by ˙ v a = u b ∇ b v a = v b ∇ b u a = B a b v b = 1 3 θv a + σ a b v b + ω a b v b for B a b := ∇ b u a where we have used the fact that the vector fields u and v commute. It follows from this that the length of v changes by d dλ  v  = 1  v  ( 1 3 θv 2 + σ ab v a v b ) = 1 3 θ  v  + σ ab v a v b /  v  . Now suppose that v a is one of a set of three spacial vector fields spanning the t = constant sections in a RobertsonWalker spacetime, i. e. the comoving frame. By isotropy, the shear for the flow of this vector must vanish, for if it did not, a round sphere at t = t would evolve into a squashed sphere for t > t which is certainly not invariant under rotations about its center. Hence d dλ  v  = 1 3 θ  v  . Now the metric for a RobertsonWalker spacetime can be put in the form ds 2 = dt 2 a 2 ( t ) d Σ 2 , (1) where d Σ 2 is the volume element of a unit (pseudo)sphere or Euclidean 3space. In other words, all lengths on Σ are determined by a ( t ). In particular, the spacial sections are expanding uniformly in all directions at the rate ˙ a = 1 3 θa (2) as we have just seen. 1 Consequently, ¨ a = 1 3 ( ˙ θa + 1 3 θ 2 a ). Then, by the shearless, twistless, Raychaudhuri equation, ¨ a/a = 1 3 R ab u a u b . The “tracereverse” of the standard Einstein equation, R ab 1 2 g ab R = 8 πT ab , is R ab = 8 π ( T ab 1 2 g ab T ). Futhermore, the stressenergy of a perfectly homogeneous and isotropic comoving cosmological fluid is given in the coordinate system of (1) as ( T αβ ) = diag( ρ, p, p, p ), where ρ is the energy density and p is the pressure. Plugging this in gives ¨ a a = 8 π 3 ρ 1 2 ( ρ 3 p ) = 4 π 3 ( ρ + 3 p ) , (3) 1 It is worth emphasizing here that the expansion represented by θ is that of the comoving frame or “cosmological fluid” (also known as the (in)famous “aether”)....
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 Fall '09
 Vector Space, Work, General Relativity, cosmological ﬂuid

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