Schwarzchild solution with cosmological constant

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Discussion Overview

The discussion revolves around solving for the Schwarzschild solution with a cosmological constant, exploring the mathematical framework and implications of such a solution. Participants engage with concepts related to non-linear equations and the derivation of metric components in the context of general relativity.

Discussion Character

  • Exploratory
  • Technical explanation
  • Mathematical reasoning

Main Points Raised

  • One participant expresses uncertainty about solving non-linear equations and mentions that the problem reduces to R = -4(cosmological constant), complicating simplification efforts.
  • Another participant suggests looking into the Schwarzschild-de Sitter solution and references a specific eprint that discusses modeling aspects of bound systems in this geometry.
  • A third participant describes a method for deriving the Schwarzschild-de Sitter lambdavacuum, stating that the Einstein tensor must take a specific form in lambda vacuum solutions and outlines a process for determining metric functions.
  • A question is raised about the necessity of knowledge in non-linear equations for generalizing the solution.

Areas of Agreement / Disagreement

Participants do not reach a consensus on the approach to solving the problem, and there are varying levels of understanding regarding the mathematical requirements needed for generalization.

Contextual Notes

Some assumptions about the mathematical framework and the nature of the solutions are not fully explored, particularly regarding the implications of the cosmological constant and the specific forms of the metric components.

Who May Find This Useful

This discussion may be of interest to those studying general relativity, particularly in the context of solutions involving cosmological constants and non-linear equations.

Terilien
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How do we solve for it? I still don't know much about non linear equations. Unfortunately, this reduces to R=-4(cosmos constant) which is not a system thus making simplicfication difficult. I'm assuming that we can still use the previous arguments and assume that the metric coompontents Gtt and Grr are exponential functions but beyond that I'm not sure what to do...
 
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You might look at the Schwarzschild - de Sitter solution, for instance http://arxiv.org/abs/gr-qc/0602002. This eprint doesn't go into the "how" of the solution very much (in fact it's concerned about modelling aspects of bound systems in such a geometry). If you really want "how" and not just a solution, I'd try Wald. I believe his approach to finding the Schwarzschild solution could be easily generalized to finding the Schwarzschild solution with a cosmological constant.
 
Deriving the Schwarzschild-de Sitter lambdavacuum

pervect said:
I believe his approach to finding the Schwarzschild solution could be easily generalized to finding the Schwarzschild solution with a cosmological constant.

Yeah, it's trivial. You know that in any lambda vacuum solution, the Einstein tensor (evaluated wrt some frame field) has to have the form k \, \operatorname{diag}(-1,1,1,1) where k is some undetermined constant. So start with a Schwarzschild coordinate chart (having two undetermined functions) and plug in this condition. The EFE then reduces to a simple ODE similar to the one you obtain in solving for the Schwarzschild vacuum; indeed the case k=0 recovers the Schwarzschild vacuum. This determines both metric functions up to constant multiples which can be "gauged away". Now you can relate the parameter k to either the "cosmological horizon radius" or equivalently to the "cosmological constant". The resulting solution is properly called the "Schwarzschild-de Sitter lambdavacuum". Historically-minded writers sometimes call it "Kottler solution".
 
Question, will i need some knowledge of non linear equations, to generalize it?
 

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