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:

Related to Form of radial velocity along null geodesic under the Kerr metric

What is the Kerr metric?

The Kerr metric describes the geometry of spacetime around a rotating massive object, such as a rotating black hole. It is a solution to Einstein's field equations of general relativity and generalizes the Schwarzschild metric, which describes a non-rotating massive object.

What is a null geodesic?

A null geodesic is the path that light (or any massless particle) follows through spacetime. In the context of the Kerr metric, null geodesics describe the trajectories of photons in the gravitational field of a rotating black hole.

How is radial velocity defined along a null geodesic in the Kerr metric?

Radial velocity along a null geodesic in the Kerr metric refers to the rate of change of the radial coordinate (r) with respect to an affine parameter (such as proper time for a massive particle or an analogous parameter for a massless particle) along the path of the light. It is derived from the geodesic equations specific to the Kerr spacetime.

Why is studying radial velocity along null geodesics important?

Studying radial velocity along null geodesics is crucial for understanding the behavior of light near rotating black holes. This has implications for astrophysical phenomena such as gravitational lensing, the shadow of black holes, and the dynamics of accretion disks around black holes.

What are the key equations involved in determining radial velocity along null geodesics in the Kerr metric?

The key equations involve the Kerr metric components and the geodesic equations. Specifically, the equations for the radial coordinate (r) and the time coordinate (t) must be solved simultaneously. These equations typically include the conserved quantities of energy and angular momentum for the photon, and they can be expressed in terms of the Boyer-Lindquist coordinates used in the Kerr metric.

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