Schwarzschild metric in 3-dimensional space-time

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SUMMARY

The discussion centers on the derivation of the Schwarzschild solution in 3-dimensional space-time, specifically addressing the challenges in adapting the 4-dimensional solution to a 3-dimensional context. Participants confirm that the Schwarzschild solution in 3D without a cosmological constant results in a flat metric, as evidenced by calculations of the Ricci tensor yielding zero. The conversation also highlights the absence of black hole solutions in 2 or 3 dimensions, reinforcing the conclusion that the Schwarzschild solution does not apply in these cases.

PREREQUISITES
  • Understanding of general relativity and Einstein's field equations.
  • Familiarity with the Schwarzschild metric and its derivation.
  • Knowledge of Ricci tensor calculations and their implications in vacuum solutions.
  • Experience with symbolic computation tools like Maxima for tensor calculations.
NEXT STEPS
  • Explore the implications of the BTZ black hole in 2+1 dimensions.
  • Study the Schwarzschild–Tangherlini metric for dimensions greater than four.
  • Investigate the role of cosmological constants in higher-dimensional general relativity.
  • Learn about the mathematical foundations of differential geometry as applied to general relativity.
USEFUL FOR

The discussion is beneficial for theoretical physicists, mathematicians specializing in general relativity, and researchers exploring gravitational theories in lower dimensions.

  • #31
As Dickfore points out, the 3D Einstein equation has a completely different physical character than the 4D one. All degrees of freedom in the curvature are locally determined by the matter distribution. This means, for example, that there can be no gravitational radiation. And there can be no analog of the Schwarzschild solution.

What might be more interesting is to look at a 2+1 slice of a static, vacuum, cylindrically symmetric 3+1 solution. This describes the Levi-Civita metric:
<br /> ds^2 = - \rho^{4 \alpha} d t^2 + \rho^{4 \alpha (2 \alpha-1)} ( d \rho^2 + d z^2 ) + \beta^{-2} \rho^{2-4\alpha} d \phi^2 .<br />
\alpha can be interpreted as a mass/length and \beta is an angular defect parameter.
 

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