Kerr metric hydrostatic equilibrium

[Orion1]

I basically understand how the Tolman-Oppenheimer-Volkoff equation for hydrostatic equilibrium was derived from the Schwarzschild metric in General Relativity and from the equation derivatives listed. However, when I attempt to derive the equation derivatives for the Kerr metric, I obtain these extremely large solutions which do not contain any derivatives.

Has the relative analogous equivalent to the Tolman-Oppenheimer-Volkoff equation for hydrostatic equilibrium for the Kerr metric ever been derived?

I am not specifically interested in the proof, only the solution. Although it would be very interesting to examine the proof.

Schwarzschild metric line element:
ds^2 = e^{\nu (r)} c^2 dt^2 - e^{\lambda (r)} dr^2 - r^2 ( \sin^2 \theta d \phi^2 + d \theta^2)

General Relativity:
G_{\mu \nu} = \frac{8 \pi G}{c^4} T_{\mu \nu}

Equation derived from Einstein tensor matrix element T_{11}:
\frac{8 \pi G P(r)}{c^4} = e^{- \lambda} \left( \frac{1}{r} \frac{d \nu}{dr} + \frac{1}{r^2} \right) - \frac{1}{r^2}

e^{-\lambda} = r^{-1}(r - r_s)

Hydrostatic equilibrium equation derived from Einstein tensor matrix elements T_{11} and T_{22}:
\frac{d \nu}{dr} = \frac{2}{P(r) + \rho(r) c^2} \left( \frac{dP(r)}{dr} \right)

Hydrostatic equilibrium:
\frac{dP(r)}{dr} = - \left( P(r) + \rho(r)c^2 \right) \frac{d \phi}{dr}

Tolman-Oppenheimer-Volkoff equation:
\boxed{\frac{dP(r)}{dr} = -(P(r) + \rho(r) c^2) \left( \frac{4 \pi G r^3 P(r)}{c^4} + \frac{r_s}{2} \right) \left[ r \left( r - r_s \right) \right]^{-1}} \; \; \; (r > r_p) \; \; \; r \neq r_p

The Kerr metric line element:
c^{2} d\tau^{2} = \left( 1 - \frac{r_{s} r}{\rho^{2}} \right) c^{2} dt^{2} - \frac{\rho^{2}}{\Lambda^{2}} dr^{2} - \rho^{2} d\theta^{2} - \left( r^{2} + \alpha^{2} + \frac{r_{s} r \alpha^{2}}{\rho^{2}} \sin^{2} \theta \right) \sin^{2} \theta \ d\phi^{2} + \frac{2r_{s} r\alpha \sin^{2} \theta }{\rho^{2}} \, c \, dt \, d\phi

General Relativity Kerr metric tensor matrix elements:
g_{\mu \nu} = \left( \begin{array}{llll} 1 - \frac{r r_s}{r^2+\alpha ^2 \cos ^2(\theta )} & 0 & 0 & \frac{r \alpha \sin ^2(\theta ) r_s}{r^2+\alpha ^2 \cos ^2(\theta )} \\ 0 & -\frac{r^2+\alpha ^2 \cos ^2(\theta )}{r^2-r_s r+\alpha ^2} & 0 & 0 \\ 0 & 0 & -r^2-\alpha ^2 \cos ^2(\theta ) & 0 \\ \frac{r \alpha \sin ^2(\theta ) r_s}{r^2+\alpha ^2 \cos ^2(\theta )} & 0 & 0 & \sin ^2(\theta ) \left(-r^2-\frac{\alpha ^2 \sin ^2(\theta ) r_s r}{r^2+\alpha ^2 \cos ^2(\theta )}-\alpha ^2\right) \end{array} \right)

Mathematica source code used by application in reference 1:

ToFileName[{$TopDirectory, "AddOns", "Applications"}]
<< einsteintensor.m
x = {t, r, \[Theta], \[Phi]}
(metric = {{1 - (Subscript[r, s]*r)/(r^2 + \[Alpha]^2*Cos[\[Theta]]^2), 0, 0, (Subscript[r, s]*r*\[Alpha]*Sin[\[Theta]]^2)/(r^2 + \[Alpha]^2*Cos[\[Theta]]^2)}, {0, -((r^2 + \[Alpha]^2*Cos[\[Theta]]^2)/(r^2 - Subscript[r, s]*r + \[Alpha]^2)), 0, 0}, {0, 0, -(r^2 + \[Alpha]^2*Cos[\[Theta]]^2), 0}, {(Subscript[r, s]*r*\[Alpha]*Sin[\[Theta]]^2)/(r^2 + \[Alpha]^2*Cos[\[Theta]]^2), 0, 0, -(r^2 + \[Alpha]^2 + (Subscript[r, s]*r*\[Alpha]^2*Sin[\[Theta]]^2)/(r^2 + \[Alpha]^2*Cos[\[Theta]]^2))*Sin[\[Theta]]^2}}) // MatrixForm
(tensor = {{\[Rho][r]*c^2, 0, 0, Subscript[\[CapitalPhi], \[Epsilon]][r]}, {0, -P[r], 0, 0},{0, 0, -P[r], 0}, {Subscript[\[Rho], p][r], 0, 0, -P[r]}}) // MatrixForm
(Einstein = Inverse[metric].Simplify[EinsteinTensor[metric, x], TimeConstraint -> 3600]) // MatrixForm
MaxMemoryUsed[]

[/Color]
Reference:
http://library.wolfram.com/infocenter/MathSource/162/"
http://en.wikipedia.org/wiki/Kerr_metric"
http://en.wikipedia.org/wiki/Schwarzschild%20metric"
http://en.wikipedia.org/wiki/Tolman-Oppenheimer-Volkoff_equation"
https://www.physicsforums.com/showpost.php?p=1801307&postcount=59"
https://www.physicsforums.com/attachment.php?attachmentid=14705&d=1216037026"

 

[atyy]

I thought the TOV equation was derived by considering how matter in a spherical star might behave, then joining it to the Schwarzschild vacuum solution outside because of Birkhoff's theorem? Or are you referring to the Schwarzschild constant density solution? I think the equation you listed for the Schwarzschild line element is for a rotationally symmetric spacetime, which would be more general than either the Schwarzschild vacuum or constant density solutions.