# Boyer–Lindquist coordinates

In the mathematical description of general relativity, the Boyer–Lindquist coordinates[1] are a generalization of the coordinates used for the metric of a Schwarzschild black hole that can be used to express the metric of a Kerr black hole.

The Hamiltonian for particle motion in Kerr spacetime is separable in Boyer–Lindquist coordinates. Using Hamilton–Jacobi theory one can derive a fourth constant of the motion known as Carter's constant.[2]

The 1967 paper introducing Boyer–Lindquist coordinates[1] was a posthumous publication for Robert H. Boyer, who was killed in the 1966 University of Texas tower shooting.[3][4]

## Line element

The line element for a black hole with a total mass equivalent ${\displaystyle M}$, angular momentum ${\displaystyle J}$, and charge ${\displaystyle Q}$ in Boyer–Lindquist coordinates and geometrized units (${\displaystyle G=c=1}$) is

${\displaystyle ds^{2}=-{\frac {\Delta }{\rho ^{2}}}\left(dt-a\sin ^{2}\theta \,d\phi \right)^{2}+{\frac {\sin ^{2}\theta }{\rho ^{2}}}{\Big (}\left(r^{2}+a^{2}\right)\,d\phi -a\,dt{\Big )}^{2}+{\frac {\rho ^{2}}{\Delta }}dr^{2}+\rho ^{2}\,d\theta ^{2}}$

where

${\displaystyle \Delta =r^{2}-2Mr+a^{2}+Q^{2},}$ called the discriminant,
${\displaystyle \rho ^{2}=r^{2}+a^{2}\cos ^{2}\theta ,}$

and

${\displaystyle a={\frac {J}{M}},}$ called the Kerr parameter.

Note that in geometrized units ${\displaystyle M}$, ${\displaystyle a}$, and ${\displaystyle Q}$ all have units of length. This line element describes the Kerr–Newman metric. Here, ${\displaystyle M}$ is to be interpreted as the mass of the black hole, as seen by an observer at infinity, ${\displaystyle J}$ is interpreted as the angular momentum, and ${\displaystyle Q}$ the electric charge. These are all meant to be constant parameters, held fixed. The name of the discriminant arises because it appears as the discriminant of the quadratic equation bounding the time-like motion of particles orbiting the black hole, i.e. defining the ergosphere.

The coordinate transformation from Boyer–Lindquist coordinates ${\displaystyle r}$, ${\displaystyle \theta }$, ${\displaystyle \phi }$ to Cartesian coordinates ${\displaystyle x}$, ${\displaystyle y}$, ${\displaystyle z}$ is given (for ${\displaystyle m\to 0}$) by:[5] {\displaystyle {\begin{aligned}x&={\sqrt {r^{2}+a^{2}}}\sin \theta \cos \phi \\y&={\sqrt {r^{2}+a^{2}}}\sin \theta \sin \phi \\z&=r\cos \theta \end{aligned}}}

## Vierbein

The vierbein one-forms can be read off directly from the line element:

${\displaystyle \sigma ^{0}={\frac {\sqrt {\Delta }}{\rho }}\left(dt-a\sin ^{2}\theta \,d\phi \right)}$
${\displaystyle \sigma ^{1}={\frac {\rho }{\sqrt {\Delta }}}dr}$
${\displaystyle \sigma ^{2}=\rho \,d\theta }$
${\displaystyle \sigma ^{3}={\frac {\sin \theta }{\rho }}{\Big (}\left(r^{2}+a^{2}\right)\,d\phi -a\,dt{\Big )}}$

so that the line element is given by

${\displaystyle ds^{2}=\sigma ^{a}\otimes \sigma ^{b}\eta _{ab}}$

where ${\displaystyle \eta _{ab}}$ is the flat-space Minkowski metric.

## Spin connection

The torsion-free spin connection ${\displaystyle \omega ^{ab}}$ is defined by

${\displaystyle d\sigma ^{a}+\omega ^{ab}\wedge \sigma ^{c}\eta _{bc}=0}$

The contorsion tensor gives the difference between a connection with torsion, and a corresponding connection without torsion. By convention, Riemann manifolds are always specified with torsion-free geometries; torsion is often used to specify equivalent, flat geometries.

The spin connection is useful because it provides an intermediate way-point for computing the curvature two-form:

${\displaystyle R^{ab}=d\omega ^{ab}+\omega ^{ac}\wedge \omega ^{db}\eta _{cd}}$

It is also the most suitable form for describing the coupling to spinor fields, and opens the door to the twistor formalism.

All six components of the spin connection are non-vanishing. These are:[6]

${\displaystyle \omega ^{01}={\frac {1}{\rho ^{3}}}\left[{\frac {-2Mr^{2}+2rQ^{2}+a^{2}[M+r+(M-r)\cos 2\theta ]}{2{\sqrt {\Delta }}}}\,\sigma ^{0}+ra\sin \theta \,\sigma ^{3}\right]}$
${\displaystyle \omega ^{02}={\frac {a\cos \theta }{\rho ^{3}}}\left[a\sin \theta \,\sigma ^{0}+{\sqrt {\Delta }}\,\sigma ^{3}\right]}$
${\displaystyle \omega ^{03}={\frac {a}{\rho ^{3}}}\left[r\sin \theta \,\sigma ^{1}-{\sqrt {\Delta }}\cos \theta \,\sigma ^{2}\right]}$
${\displaystyle \omega ^{12}={\frac {1}{\rho ^{3}}}\left[a^{2}\sin \theta \cos \theta \,\sigma ^{1}+r{\sqrt {\Delta }}\,\sigma ^{2}\right]}$
${\displaystyle \omega ^{13}={\frac {r}{\rho ^{3}}}\left[a\sin \theta \,\sigma ^{0}+{\sqrt {\Delta }}\,\sigma ^{3}\right]}$
${\displaystyle \omega ^{23}={\frac {\cot \theta }{\rho ^{3}}}\left[a{\sqrt {\Delta }}\sin \theta \,\sigma ^{0}+(r^{2}+a^{2})\,\sigma ^{3}\right]}$

## Riemann and Ricci tensors

The Riemann tensor written out in full is quite verbose; it can be found in Frè.[6] The Ricci tensor takes the diagonal form:

${\displaystyle {\mbox{Ric}}={\frac {Q^{2}}{\rho ^{4}}}{\begin{bmatrix}1&0&0&0\\0&-1&0&0\\0&0&1&0\\0&0&0&1\\\end{bmatrix}}}$

Notice the location of the minus-one entry: this comes entirely from the electromagnetic contribution. Namely, when the electromagnetic stress tensor ${\displaystyle F_{ab}}$ has only two non-vanishing components: ${\displaystyle F_{01}}$ and ${\displaystyle F_{23}}$, then the corresponding energy–momentum tensor takes the form

${\displaystyle T^{\mbox{Maxwell}}={\frac {F_{01}^{2}+F_{23}^{2}}{4}}{\begin{bmatrix}1&0&0&0\\0&-1&0&0\\0&0&1&0\\0&0&0&1\\\end{bmatrix}}}$

Equating this with the energy–momentum tensor for the gravitational field leads to the Kerr–Newman electrovacuum solution.

## References

1. ^ a b Boyer, Robert H.; Lindquist, Richard W. (1967). "Maximal Analytic Extension of the Kerr Metric". Journal of Mathematical Physics. 8 (2): 265–281. Bibcode:1967JMP.....8..265B. doi:10.1063/1.1705193.
2. ^ Carter, Brandon (1968). "Global structure of the Kerr family of gravitational fields". Physical Review. 174 (5): 1559–1571. Bibcode:1968PhRv..174.1559C. doi:10.1103/PhysRev.174.1559.
3. ^ "The Victims". Behind the Tower. 15 July 2016. Retrieved 2 November 2022.
4. ^ "Robert Hamilton Boyer". Physics Today. 19 (9): 121. September 1966. doi:10.1063/1.3048457.
5. ^ Matt Visser, arXiv:0706.0622v3, eqs. 60-62
6. ^ a b Pietro Giuseppe Frè, "Gravity, a Geometrical Course, Volume 2: Black Holes, Cosmology and Introduction to Supergravity", (2013) Springer-Verlag
• Shapiro, S. L.; Teukolsky, S. A. (1983). Black Holes, White Dwarfs, and Neutron Stars: The Physics of Compact Objects. New York: Wiley. p. 357. ISBN 9780471873167.