By energy conservation, show the 4-velocity of dust satisfies this....

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SUMMARY

The discussion focuses on demonstrating that the 4-velocity ##u^{\mu}## of dust satisfies the equation ##u^{\mu}\nabla_{\mu}u^{\nu} = f u^{\nu}##, where ##f## is a function of ##u^{\mu}##, ##\rho##, and their derivatives. The equation simplifies to ##\dot{\rho} + 3 \left(\frac{\dot{a}}{a}\right)\rho = 0## for comoving observers in a homogeneous Friedmann-Robertson-Walker Universe. The participant expresses uncertainty about treating the density ##\rho## and whether its derivative ##\nabla_{\mu} \rho## is zero. The use of the energy conservation equation ##\nabla_{\mu}T^{\mu\nu} = 0## is also discussed, highlighting the relationship between the energy density and the 4-velocity.

PREREQUISITES
  • Understanding of 4-velocity in general relativity
  • Familiarity with the Friedmann-Robertson-Walker (FRW) metric
  • Knowledge of energy-momentum tensors, specifically for dust: ##T^{\mu\nu} = \rho u^{\mu}u^{\nu}##
  • Concept of covariant derivatives and their application in general relativity
NEXT STEPS
  • Study the derivation of the Friedmann equations in cosmology
  • Learn about covariant differentiation and its implications in general relativity
  • Explore the implications of energy conservation in cosmological models
  • Investigate the behavior of density perturbations in a homogeneous universe
USEFUL FOR

Students and researchers in theoretical physics, particularly those focusing on cosmology and general relativity, will benefit from this discussion. It is especially relevant for those studying the dynamics of dust in expanding universes.

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Homework Statement


Using conservation of energy, show that the 4-velocity ##u^{\mu}## of dust satisfies:
##u^{\mu}\nabla_{\mu}u^{\nu} = f u^{\nu}##

Explicitly identify ##f##, which is some function of ##u^{\mu}##, ##\rho## and their derivatives. And show that this equation becomes

##\dot{\rho} + 3 \left(\frac{\dot{a}}{a}\right)\rho = 0##

For comoving observers in a homogeneous Friedmann-Robertson-Walker Universe.

Homework Equations

The Attempt at a Solution


I don't think I've done the first bit right, I'm not really sure how to treat the ##\rho##. For dust, ##T^{\mu\nu} = \rho u^{\mu}u^{\nu}## and energy conservation means:
##\nabla_{\mu}T^{\mu\nu} = 0##
So
##\nabla_{\mu} (\rho u^{\mu}u^{\nu})##
Using the product rule,
##\rho u^{\mu} (\nabla_{\mu}u^{\nu}) + \rho u^{\nu} (\nabla_{\mu}u^{\mu}) + u^{\mu}u^{\nu}\nabla_{\mu}\rho = 0##
I think ##\nabla_{\mu} \rho =0##, but if it is then I could just divide through by ##\rho## and I could rearrange to get the LHS
I want:
##u^{\mu}\nabla_{\mu}u^{\nu}##
But the RHS wouldn't be a function of ##\rho##. So if ##\nabla_{\mu} \rho## isn't zero, then I get:
##u^{\mu}\nabla_{\mu}u^{\nu} = -u^{\nu}\nabla_{\mu}u^{\mu} - \frac{u^{\nu}u^{\mu}}{\rho} \nabla_{\mu}\rho##
##= \left(-\nabla_{\mu}u^{\mu}-\frac{u^{\mu}}{\rho}\nabla_{\mu}\rho \right)u^{\nu}##
Is that right? Is ##\nabla_{\mu}\rho## not zero?
 
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For the second part, I'm not really sure how to do it. I think it's a case of using the FLRW metric and the equations of motion for an FRW universe?
 

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