Form of radial velocity along null geodesic under the Kerr metric

  • #1
Bertin
11
6
Homework Statement
Given the affine parameter [itex]\lambda[/itex] of a null geodesic on the equator ([itex]\theta = \pi/2[/itex]), prove that that the [itex]r[/itex] coordinate satisfies the following equation:
$$\left(\frac{dr}{d\lambda}\right)^2 = \frac{\Sigma^2}{\rho^4}(E - L W_-(r))(E - L W_+(r))$$
for some [itex]W(r)[/itex] that might depend on [itex]E,L[/itex] and [itex]r[/itex], and for [itex]E, L[/itex] constants of motion.
Relevant Equations
The Kerr metric, in the Boyer-Lindquist coordinates and on the equator, reads
$$ds^2 = -(1 - \frac{R}{r})dt^2 - \frac{R}{r}a (dtd\phi + d\phi dt) + \frac{r^2}{r^2 + a^2 - R r} dr^2 + \frac{\Sigma^2}{r^2} d\phi^2$$
for [itex]\Sigma^2 = r^4 + a^2 r^2 + R r a[/itex].
By the symmetries of the metric, [itex]k = \partial_t[/itex] and [itex]l = \partial_\phi[/itex] are Killing vectors. Since they are Killing vectors, they satisfy [itex]k_\mu \dot{x}^\mu = E[/itex] and [itex]l_\mu \dot{x}^\mu = L[/itex], for the same constants appearing in the expression we must prove, and where the dot means the derivative w.r.t. to the affine parameter. Hence it follows that
$$E = -(1 - \frac{R}{r})\dot{t} - \frac{R}{r}a\dot{\phi}$$
$$L = -\frac{R}{r}a\dot{t} + \frac{\Sigma^2}{r^2}\dot{\phi}$$.
Moreover, since [itex]x(\lambda)[/itex] is a null geodesic, we have that [itex]\dot{x}_\mu\dot{x}^\mu = 0[/itex], whence
$$ 0 = \frac{r^2}{r^2 + a^2 - R r}\dot{r}^2 - (1 - \frac{R}{r})\dot{t}^2 - 2\frac{R}{r}a\dot{t}\dot{\phi} + \frac{\Sigma^2}{r^2}\dot{\phi}^2$$

We can then solve the equations of [itex]E[/itex] and [itex]L[/itex] for [itex]\dot{t}[/itex] and [itex]\dot{\phi}[/itex] to later replace those values inside last equation. Nevertheless, this leads to a very messy expression for [itex]\dot{r}^2[/itex] that does not look that the one we must prove, first and foremost because the resulting expression doesn't seem to include any [itex]\frac{\Sigma^2}{r^4}E^2[/itex] (unless both Mathematica and I are missing a possible simplification, which could be the case), so I probably have done some mistake (not calculatory, though, because my results agree with Mathematica) or I am missing something.

I would appreciate if someone could show me how do we derive above expression. Thank you in advance.
 
Last edited:

What is the form of radial velocity along null geodesic under the Kerr metric?

The form of radial velocity along null geodesic under the Kerr metric can be described by the equation: $V_r = \pm \sqrt{\frac{R(r)}{g_{\phi\phi}}}$. Here, $V_r$ represents the radial velocity, $R(r)$ is the function of $r$ in the Kerr metric, and $g_{\phi\phi}$ is the metric component related to the azimuthal direction.

How does the form of radial velocity along null geodesic change in the Kerr metric compared to other metrics?

In the Kerr metric, the form of radial velocity along null geodesic is influenced by the presence of the angular momentum of the rotating black hole. This results in a modification to the expression for radial velocity compared to other metrics, where the impact of the black hole's rotation is taken into account.

What are the key factors that determine the form of radial velocity along null geodesic under the Kerr metric?

The key factors that determine the form of radial velocity along null geodesic under the Kerr metric include the specific parameters of the Kerr black hole, such as its mass and angular momentum, as well as the radial distance from the black hole. These factors contribute to the overall shape and behavior of the radial velocity along null geodesic in the Kerr metric.

How is the form of radial velocity along null geodesic under the Kerr metric relevant in the study of black holes?

The form of radial velocity along null geodesic under the Kerr metric is crucial in understanding the dynamics of particles and light near rotating black holes. By analyzing the radial velocity along null geodesic, researchers can gain insights into the gravitational effects of Kerr black holes and their impact on the motion of objects in their vicinity.

Can the form of radial velocity along null geodesic under the Kerr metric be experimentally verified?

While the theoretical form of radial velocity along null geodesic under the Kerr metric can be derived using mathematical equations, experimental verification of this phenomenon is challenging due to the extreme conditions near black holes. However, advancements in observational techniques and technology may eventually allow for indirect verification of the predicted radial velocity behavior in the vicinity of Kerr black holes.

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