Near-Horizon Metric: Understanding Equation 4.2

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In summary, the conversation discusses the article on general Kerr-de Sitter metrics and the statement made by the authors after Equation 4.2. The person is struggling to understand the reason behind the statement and is looking for help. They are advised to look at Kerr Solution or Kerr Neumann Metric and Killing vector fields, which become null at the event horizon. The conversation concludes with the realization that the statement is related to the rotating reference frame.
  • #1
vizart
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I am reading this article http://arxiv.org/abs/hep-th/0404008 on general Kerr-de Sitter metrics.
It seems to be obvious, but I can't see the reason behind the statement that authors make after Equation 4.2 that "As the horizon is approached, the right-hand side of (4.2) approaches zero."
I would be appreciative if somebody could help me with this issue.
 
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  • #2
You might try Wikipedia for a clue,,,
Kerr Solution or Kerr Neumann Metric..
 
  • #3
Naty1 said:
You might try Wikipedia for a clue,,,
Kerr Solution or Kerr Neumann Metric..

thank you for the tip but if you look at the Boyer-Lindquist form #(4.1), you see that it is quite general and i think their statement is somehow related to the fact that the horizon is a null hypersurface. yet i don't know the 'how' part :)
 
  • #5
I must be hanged for not seeing the simple fact that when the metric has the given Lewis form (4.1) if you move to the rotating reference frame, then the near-horizon condition "RHS of Eqn. 4.2 approaches zero" will be obvious.
 

FAQ: Near-Horizon Metric: Understanding Equation 4.2

What is the Near-Horizon Metric?

The Near-Horizon Metric is a mathematical equation used in black hole physics to describe the spacetime geometry near the event horizon of a black hole. It is part of the larger framework of General Relativity.

What does Equation 4.2 represent in the Near-Horizon Metric?

Equation 4.2 is a specific form of the Near-Horizon Metric that is often used to study the properties of black holes. It represents the spacetime geometry near the event horizon of a stationary black hole.

How is the Near-Horizon Metric derived?

The Near-Horizon Metric is derived from the Einstein field equations of General Relativity. It involves solving a set of differential equations and making simplifying assumptions about the properties of a black hole near its event horizon.

What is the significance of the Near-Horizon Metric in black hole physics?

The Near-Horizon Metric allows scientists to study the properties of black holes, such as their mass and spin, near their event horizons. It is also important in understanding the behavior of matter and light as they approach the event horizon of a black hole.

Are there any limitations to the Near-Horizon Metric?

Like any mathematical model, the Near-Horizon Metric has its limitations. It assumes a stationary black hole and does not take into account the effects of quantum mechanics. It also does not apply to black holes that are rapidly spinning or merging with other black holes.

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