The observed angular velocity of the frame drag in the system of the coordinate bookkeeper far away from the mass is^[1]

${\displaystyle {\rm {\omega ={\frac {2\ a\ r}{\Xi }}}}}$

in units of ${\displaystyle {\rm {G=M=c=1}}}$ and with

${\displaystyle {\rm {\Sigma =r^{2}+a^{2}\ \cos ^{2}\theta ,\ \Delta =r^{2}-2\ r+a^{2},\ \Xi =\left(a^{2}+r^{2}\right)^{2}-a^{2}\ \sin ^{2}\theta \ \Delta }}}$

The radius of gyration is given by^[2]

${\displaystyle {\rm {{\bar {R}}={\sqrt {\frac {\Xi }{\Sigma }}}}}}$

and the cartesian coordinates in the bookkeeper's frame of reference are

${\displaystyle {\rm {r_{xy}={\sqrt {(a^{2}+r^{2})\sin ^{2}\theta }}}},\ {\rm {r_{xyz}}}={\rm {\sqrt {r_{xy}^{2}+r^{2}\cos ^{2}\theta }}}}$

The gravitational time dilation component is

${\displaystyle {\rm {\varsigma ={\sqrt {\frac {\Xi }{\Sigma \ \Delta }}}}}}$

so the observed transverse velocity of a frame dragged zero angular momentum probe is

${\displaystyle {\rm {u_{\perp }=\Omega _{obs}=\omega \ r_{xy}}}}$

and the local velocity

${\displaystyle {\rm {v_{\perp }=\Omega _{loc}=\omega \ {\bar {R}}\ \varsigma }}}$

That is exactly the speed of light at the outer edge of the outer ergosphere at

${\displaystyle {\rm {r_{\text{ergo}}=1+{\sqrt {1-a^{2}\cos ^{2}\theta }}}}}$

which corresponds to a Boyer-Lindquist radius of ${\displaystyle 2}$ and a cartesian radius of ${\displaystyle {\sqrt {\rm {2^{2}+a^{2}}}}}$ at the equator.

1. ↑ Andrei & Valeri Frolov: Rigidly rotating ZAMO surfaces in the Kerr spacetime, page 1, eq. 5
2. ↑ Scott A. Hughes: Nearly horizon skimming orbits of Kerr black holes, pages 5, 6 etc

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• de.wikipedia.org/wiki/Kerr-Metrik
• de.wikipedia.org/wiki/Lense-Thirring-Effekt
• en.wikipedia.org/wiki/Lense-Thirring_precession