Wahlquist fluid

The Wahlquist fluid was first discovered by Hugo D. Wahlquist in 1968.[1] It is one of few known exact rotating perfect fluid solutions in general relativity. The solution reduces to the static Whittaker metric in the limit of zero rotation.

The metric of a Wahlquist fluid is given by

${\displaystyle ds^{2}=f(dt-{\tilde {A}}d\varphi )^{2}-r_{0}^{2}(\zeta ^{2}+\xi ^{2})[{\frac {d\zeta ^{2}}{(1-{\tilde {k}}^{2}\zeta ^{2}){\tilde {h}}_{1}}}+{\frac {d\xi ^{2}}{(1+{\tilde {k}}^{2}\xi ^{2}){\tilde {h}}_{2}}}+{\frac {{\tilde {h}}_{1}{\tilde {h}}_{2}}{{\tilde {h}}_{1}-{\tilde {h}}_{2}}}d\varphi ^{2}]}$

where

${\displaystyle f={\frac {{\tilde {h}}_{1}-{\tilde {h}}_{2}}{\zeta ^{2}+\xi ^{2}}}}$

${\displaystyle {\tilde {A}}=r_{0}({\frac {\xi ^{2}{\tilde {h}}_{1}+\zeta ^{2}{\tilde {h}}_{2}}{{\tilde {h}}_{1}-{\tilde {h}}_{2}}}-\xi _{A}^{2})}$

${\displaystyle {\tilde {h}}_{1}(\zeta )=1+\zeta ^{2}+{\frac {\zeta }{\kappa ^{2}}}[\zeta _{+}{\frac {1}{\tilde {k}}}{\sqrt {1-{\tilde {k}}^{2}\zeta ^{2}}}\arcsin({\tilde {k}}\zeta )]}$

${\displaystyle {\tilde {h}}_{2}(\xi )=1-\xi ^{2}-{\frac {\xi }{\kappa ^{2}}}[\xi _{-}{\frac {1}{\tilde {k}}}{\sqrt {1+{\tilde {k}}^{2}\xi ^{2}}}\sinh ^{-1}({\tilde {k}}\xi )]}$

and ${\displaystyle \xi _{A}}$ is defined by ${\displaystyle {\tilde {h}}_{2}(\xi _{A})=0}$. It is a solution with equation of state ${\displaystyle \mu +3p=\mu _{0}}$ where ${\displaystyle \mu _{0}}$ is a constant.

The pressure and density of the Wahlquist fluid are given by

${\displaystyle p={\frac {1}{2}}\mu _{0}(1-\kappa ^{2}f)}$

${\displaystyle \mu ={\frac {1}{2}}\mu _{0}(3\kappa ^{2}f-1)}$

The vanishing pressure surface of the fluid is prolate, in contrast to physical rotating stars, which are oblate. It has been shown that the Wahlquist fluid can not be matched to an asymptotically flat region of spacetime.[2]