How Long Does It Take to Fall into a 5-D Black Hole?

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The discussion focuses on calculating the time it takes for an observer to fall into a 5-D black hole, starting from rest at a specific radial distance. The user attempts to use Lemaitre coordinates to eliminate singularities in the metric but expresses uncertainty about the integration step to find the elapsed time. Responses highlight potential errors in the user's equations, particularly regarding the coefficients in the line element and the conditions for radial free-fall. Suggestions are made to revert to Schwarzschild coordinates for clarity, noting that the derivation for time in 5-D should parallel that of 4-D with necessary adjustments. The conversation emphasizes the importance of correctly applying the metric and integration methods to determine the fall time accurately.
Confused Physicist
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Hi, I have the following problem:

Given the 5-D generalization of the Schwarszschild solution with line element:

ds^2=-\Bigg(1-\frac{r^2_+}{r^2}\Bigg)dt^2+\Bigg(1-\frac{r^2_+}{r^2}\Bigg)^{-1}dr^2+r^2[d\chi^2+\sin^2(\chi)(d\theta^2+\sin^2(\theta)d\phi^2)]

where ##r_+## is a positive constant. An observer falls radially starting from rest at ##r=10r_+##. How much time elapses on their clock before they hit the singularity at ##r=0##?

MY ATTEMPT HAS BEEN:

Using the Lemaitre coordinates ##\tau##, ##\rho## to eliminate the singularity of ##ds^2## at ##r_+##:

d\tau=dt+\frac{r_+}{r}\frac{dr}{1-\frac{r^2_+}{r^2}}

d\rho=dt+\frac{r}{r_+}\frac{dr}{1-\frac{r_+^2}{r^2}}\quad\quad\quad (1)

we have the following line element where the singularity at ##r_+## is removed:

ds^2=d\tau^2-\frac{r_+}{r}d\rho^2-r^2(d\theta^2+\sin^2(\theta)d\phi^2)

where ##r=\sqrt{2(\rho-\tau)r_+}##, which is obtained by integrating d\rho-d\tau=\frac{r}{r_+}dr.

For a free falling body, ##d\rho=0##, and equation (1) gives:

dt=-\frac{r}{r_+}\frac{1}{1-\frac{r_+}{r}}dr

Integrating this equation from ##r=10r_+## to ##r=0## should give me the time the problem asks for:

\Delta\tau=-\int_{10r_+}^0 \frac{r}{r_+}\frac{1}{1-\frac{r_+}{r}}dr

Is this correct?

Thanks!
 
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I have the feeling the last step, where I integrate ##dt## and get the time the observer takes to fall into the black hole, is not quite correct. But I'm not really sure. Could someone help me out? Thanks, I really appreciate it.
 
Confused Physicist said:
Using the Lemaitre coordinates ##\tau##, ##\rho## to eliminate the singularity of ##ds^2## at ##r_+##:

d\tau=dt+\frac{r_+}{r}\frac{dr}{1-\frac{r^2_+}{r^2}}

d\rho=dt+\frac{r}{r_+}\frac{dr}{1-\frac{r_+^2}{r^2}}\quad\quad\quad (1)
Your expressions here don't appear to correspond to the usual definition of Lemaitre coordinates. You are missing some square roots. Also, should the ##r##'s be squared in the denominators? See https://en.wikipedia.org/wiki/Lemaître_coordinates

[EDIT: Sorry. I overlooked the fact that the ##r##'s are squared in the 5-D version of the metric. I'm not familiar with this. So, your expressions for the Lemaitre coordinates are probably OK.
However, I think there is a typo in your equation

ds^2=d\tau^2-\frac{r_+}{r}d\rho^2-r^2(d\theta^2+\sin^2(\theta)d\phi^2)
Shouldn't the coefficient of ##d\rho^2## on the right be ##\left(\frac{r_+}{r}\right)^2## instead of ##\frac{r_+}{r}##? You have changed the overall sign of ##ds^2## when going from the Schwarzschild coordinates to the Lemaitre coordinates. Also, here your angular part is for 4D rather than 5D.​
For a free falling body, ##d\rho=0##,
##d\rho=0## only holds for radial free-fall if the initial condition corresponds to starting at rest at infinity. For a particle that starts at rest at a finite value of ##r##, ##d\rho \neq 0##.

You can solve the problem sticking with the Schwarzschild coordinates. In standard texts, it is shown how to derive an expression for ##\frac{dt}{d \tau}## in terms of ##r## for any free-fall trajectory. Here, ##\tau## is proper time for the freely falling particle. See the first equation here: http://grwiki.physics.ncsu.edu/wiki/Schwarzschild_Black_Hole#Geodesic_Motion
I think this equation should still be valid in the 5-D spacetime of your problem.

[EDIT: The equation for ##\frac{dt}{d \tau}## will probably change for 5-D. I will try to find the time to work it out. The derivation should be similar to the 4-D derivation.]​

You can use this equation along with the form of the metric to deduce an expression for ##\frac{dr}{d \tau}## as a function of ##r## for radial motion.
 
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The 5-D case does appear to work out just as easily as the 4-D case. You should find that the expression for ##\frac{dt}{d\tau}## in the 5D case differs from the 4D case by just replacing ##\frac{r_+}{r}## in the 4D case by ##\left(\frac{r_+}{r}\right)^2##. Then, working out an expression for ##\frac{dr}{d\tau}## from the 5D metric is very similar to working it out in the 4D case. The final integration to obtain the total infall time ##\tau## is actually easier in the 5D case (if I didn't make any mistakes).
 
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