Energy-Momentum Tensor of Perfect Fluid

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SUMMARY

The discussion focuses on deriving the energy-momentum tensor for a perfect fluid within the context of a cosmological metric defined by ##ds^2 = - c^2dt^2 + a(t)^2 (dx^2 + dy^2 + dz^2)##. The non-vanishing Christoffel symbols are identified, and the energy-momentum tensor is expressed as ##T^{\alpha \beta} = \left( \rho + \frac{P}{c^2} \right)u^{\alpha}u^\beta + Pg^{\alpha \beta}##. The conservation equation leads to the result ##\frac{d(\rho a^3)}{da} + \frac{3Pa^2}{c^2} = 0##, confirming the relationship between energy density, pressure, and scale factor in cosmology.

PREREQUISITES
  • Understanding of general relativity concepts, particularly the energy-momentum tensor.
  • Familiarity with cosmological metrics and their implications.
  • Knowledge of Christoffel symbols and their role in geodesic equations.
  • Basic proficiency in differential equations and continuity equations in physics.
NEXT STEPS
  • Study the derivation of the Friedmann equations in cosmology.
  • Learn about the implications of the perfect fluid model in cosmological models.
  • Investigate the role of the scale factor ##a(t)## in the evolution of the universe.
  • Explore the relationship between energy density, pressure, and the equation of state in cosmology.
USEFUL FOR

Physicists, cosmologists, and students studying general relativity and cosmology, particularly those interested in the dynamics of perfect fluids in expanding universes.

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Homework Statement



I am given this metric: ##ds^2 = - c^2dt^2 + a(t)^2 \left( dx^2 + dy^2 + dz^2 \right)##. The non-vanishing christoffel symbols are ##\Gamma^t_{xx} = \Gamma^t_{yy} = \Gamma^t_{zz} = \frac{a a'}{c^2}## and ##\Gamma^x_{xt} = \Gamma^x_{tx} = \Gamma^y_{yt} = \Gamma^y_{ty} = \Gamma^z_{zt} = \Gamma^z_{tz} = \frac{a'}{a}##.

The energy momentum tensor can be written as ##T^{\alpha \beta} = \left( \rho + \frac{P}{c^2} \right)u^{\alpha}u^\beta + Pg^{\alpha \beta}##. Show that ##\frac{d(\rho a^3)}{da} + \frac{3Pa^2}{c^2} = 0##.

Homework Equations

The Attempt at a Solution



I shall let c=1 and u = (1,0,0,0) for simplicity.
[/B]
I know that the conservation requirement gives
\nabla_\alpha T^{\alpha \beta} = 0
Letting c=1, we have the relativistic continuity equation as
u^\alpha \left(\nabla_\alpha \rho \right) + (\rho + P)\left( \nabla_\alpha u^\alpha \right) = 0

For ##\nabla_\alpha \rho = \partial_\alpha \rho## and ##\nabla_\alpha u^\alpha = \partial_\alpha + \Gamma^\alpha_{\alpha \mu} u^\mu =\partial_\alpha u^\alpha + u^t \left( \Gamma^x_{xt} + \Gamma^y_{yt} + \Gamma^z_{zt} \right) = 3c \left( \frac{a'}{a} \right)##.

Thus we have
u^\alpha \partial_\alpha \rho + 3(\rho + P)\left( \frac{a'}{a} \right) = 0
\partial_t \rho + 3(\rho + P)\left( \frac{a'}{a} \right) = 0

How do I proceed?
 
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