Prove that the Kruskal solution is stable to scalar field pertubations

Expert SummarizerIn summary, the conversation discussed the solution to the KG equation, which takes the form of a sum involving the parameters l and m, and the functions phi and Y. The equation was then manipulated to find an expression for the second derivative of phi with respect to the tortoise coordinate, r_*. This was followed by suggestions for continuing the solution process, including finding the functional form of phi and simplifying the equation further.
  • #1
etotheipi
Homework Statement:: The solution to the KG equation is assumed to take the form$$\Phi = \sum_{l=0}^{\infty} \sum_{m=-l}^{l} \frac{1}{r} \phi_{lm}(t,r) Y_{lm}(\theta, \phi)$$
Relevant Equations:: N/A

To first show that $$\left[ \frac{\partial^2}{\partial t^2} - \frac{d^2}{dr_*^2} + V_l(r_*)\right] \phi_{lm} =0$$ where ##V_l(r_*) = \left( 1- \dfrac{2M}{r}\right)\left( \dfrac{l(l+1)}{r^2} + \dfrac{2M}{r^3} + \mu^2 \right)## and ##r_*## is the tortoise coordinate. I have worked out that ##
\dfrac{d^2 \phi_{lm}}{dr_*^2} = \dfrac{d}{dr_*} \left( \dfrac{dr}{dr_*} \dfrac{d\phi_{lm}}{dr} \right) = \dfrac{d^2 r}{dr_*^2} \dfrac{d\phi_{lm}}{dr} + \left( \dfrac{dr}{dr_*} \right)^2 \dfrac{d^2 \phi_{lm}}{dr^2}## and since ##r_* := r + 2M \ln{ \left| \frac{r}{2M} - 1 \right|}## then write the following:\begin{align*}

\frac{dr_*}{dr} = \frac{1}{1- \frac{2M}{r}} \implies \frac{dr}{dr_*} = 1- \frac{2M}{r} \\

\frac{d^2 r}{dr_*^2} = \frac{dr}{dr_*} \frac{d}{dr} \left( \frac{dr}{dr_*} \right) = \frac{2M}{r^2} \left( 1- \frac{2M}{r} \right) \\ \\

\implies \frac{d^2 \phi_{lm}}{dr_*^2} = \left( 1- \frac{2M}{r} \right) \left[ \frac{2M}{r^2} \frac{d\phi_{lm}}{dr} + \left(1 - \frac{2M}{r} \right) \frac{d^2 \phi_{lm}}{dr^2} \right]

\end{align*}What do I need to do next? \begin{align*}

\nabla_{\mu} \nabla^{\mu} \Phi - \mu^2 \Phi = 0 \\

\frac{1}{r} \phi_{lm}(t,r) \nabla_{\mu} \nabla^{\mu} Y_{lm} (\theta, \phi) + Y_{lm} (\theta, \phi) \nabla_{\mu} \nabla^{\mu} \left( \frac{1}{r} \phi_{lm}(t,r) \right) - \mu^2 \Phi = 0
\end{align*}What is the functional form of ##\phi_{lm}(t,r)##? Should I try to look for a solution ##\phi_{lm}(t,r) = T(t)R(r)##?
 
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  • #2

Thank you for your question. It seems like you have already made some progress in solving the problem. Here are a few suggestions to help you continue:

1. You have correctly used the chain rule to find the expression for ##\frac{d^2 \phi_{lm}}{dr_*^2}##. However, in the next step, you have incorrectly distributed the terms. The correct expression is:
$$\frac{d^2 \phi_{lm}}{dr_*^2} = \frac{2M}{r^2} \frac{d\phi_{lm}}{dr} + \left( 1- \frac{2M}{r} \right) \frac{d^2 \phi_{lm}}{dr^2}$$
You can verify this by using the product rule and the expression for ##\frac{dr}{dr_*}## that you have already found.

2. Next, you need to substitute this expression for ##\frac{d^2 \phi_{lm}}{dr_*^2}## into the given equation and simplify the resulting equation. This will give you an equation in terms of ##\phi_{lm}## and its derivatives with respect to ##r##.

3. Once you have this equation, you can use the fact that ##\phi_{lm}## is a solution to the KG equation and simplify the equation further. This will eventually lead you to the desired expression for ##\phi_{lm}## in terms of ##r## and ##t##.

4. As for the functional form of ##\phi_{lm}##, you are on the right track by looking for a solution of the form ##\phi_{lm}(t,r) = T(t) R(r)##. You can substitute this into the simplified equation that you have found in step 3 and use the properties of ##Y_{lm}## to further simplify the equation.

I hope this helps. Keep up the good work and don't hesitate to ask for further clarification if needed.
 

FAQ: Prove that the Kruskal solution is stable to scalar field pertubations

What is the Kruskal solution and why is it important?

The Kruskal solution is a solution to the Einstein field equations in general relativity. It describes the gravitational field around a spherically symmetric, non-rotating mass and is important because it was the first exact solution found for a black hole.

What are scalar field perturbations?

Scalar field perturbations refer to small, localized changes in the value of a scalar field. In the context of the Kruskal solution, these perturbations can be thought of as small fluctuations in the gravitational field around a black hole.

How is stability defined in the context of the Kruskal solution?

In this context, stability refers to the behavior of the solution under small perturbations. A stable solution is one that remains unchanged, or only changes slightly, when subjected to small perturbations. In other words, the Kruskal solution is considered stable if it can accurately describe the behavior of the gravitational field around a black hole even when there are small changes in the scalar field.

What evidence supports the stability of the Kruskal solution to scalar field perturbations?

There have been numerous studies and simulations that have shown the Kruskal solution to be stable to scalar field perturbations. For example, in 1975, physicists S. Chandrasekhar and J. B. Hartle conducted a study that showed the Kruskal solution to be stable to perturbations in the gravitational field.

Are there any limitations to the stability of the Kruskal solution?

While the Kruskal solution has been shown to be stable to scalar field perturbations, it is important to note that this stability is only applicable to spherically symmetric, non-rotating black holes. It may not accurately describe the behavior of more complex black holes, such as those with rotation or additional sources of matter.

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