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3+1 Einstein equations in the $\delta=2$ Tomimatsu-Sato spacetime
This worksheet is based on SageManifolds (version 0.7) and regards the 3+1 slicing of the $\delta=2$ Tomimatsu-Sato spacetime.
It is released under the GNU General Public License version 2.
(c) Claire Somé, Eric Gourgoulhon (2015)
The worksheet file in Sage notebook format is here.
Tomimatsu-Sato spacetime
The Tomimatsu-Sato solution is an exact stationary and axisymmetric solution of the vaccum Einstein equation, which is asymptotically flat and has a non-zero angular momentum. It has been found in 1972 by A. Tomimatsu and H. Sato [Phys. Rev. Lett. 29, 1344 (1972)], as a solution of the Ernst equation. It is actually the member $\delta=2$ of a larger family of solutions parametrized by a positive integer $\delta$ and exhibited by Tomimatsu and Sato in 1973 [Prog. Theor. Phys. 50, 95 (1973)], the member $\delta=1$ being nothing but the Kerr metric. We refer to [Manko, Prog. Theor. Phys. 127, 1057 (2012)] for a discussion of the properties of this solution.Â
Spacelike hypersurface
We consider some hypersurface $\Sigma$ of a spacelike foliation $(\Sigma_t)_{t\in\mathbb{R}}$ of $\delta=2$ Tomimatsu-Sato spacetime; we declare $\Sigma_t$ as a 3-dimensional manifold:
On $\Sigma$, we consider the prolate spheroidal coordinates $(x,y,\phi)$, with $x\in(1,+\infty)$, $y\in(-1,1)$ and $\phi\in(0,2\pi)$ :
Riemannian metric on $\Sigma$
The Tomimatsu-Sato metric depens on three parameters: the integer $\delta$, the real number $p\in[0,1]$, and the total mass $m$:
We set $\delta=2$ and choose a specific value for $p=1/5$:
Furthermore, without any loss of generality, we may set $m=1$ (this simply fixes some length scale):
The parameter $q$ is related to $p$ by $p^2+q^2=1$:
Some shortcut notations:
The Riemannian metric $\gamma$ induced by the spacetime metric $g$ on $\Sigma$:
A matrix view of the components w.r.t. coordinates $(x,y,\phi)$:
Lapse function and shift vector
Extrinsic curvature of $\Sigma$
We use the formula \[ K_{ij} = \frac{1}{2N} \mathcal{L}_{\beta} \gamma_{ij}, \] which is valid for any stationary spacetime:
The component $K_{13} = K_{x\phi}$:
The type-(1,1) tensor $K^\sharp$ of components $K^i_{\ \, j} = \gamma^{ik} K_{kj}$:
We may check that the hypersurface $\Sigma$ is maximal, i.e. that $K^k_{\ \, k} = 0$:
Connection and curvature
Let us call $D$ the Levi-Civita connection associated with $\gamma$:
The Ricci tensor associated with $\gamma$:
The scalar curvature $R = \gamma^{ij} R_{ij}$:
3+1 Einstein equations
Let us check that the vacuum 3+1 Einstein equations are satisfied.
We start by the constraint equations:
Hamiltonian constraint
Let us first evaluate the term $K_{ij} K^{ij}$:
The vacuum Hamiltonian constraint equation is \[R + K^2 -K_{ij} K^{ij} = 0 \]
In vacuum and for stationary spacetimes, the dynamical Einstein equations are \[ \mathcal{L}_\beta K_{ij} - D_i D_j N + N \left( R_{ij} + K K_{ij} - 2 K_{ik} K^k_{\ \, j}\right) = 0 \]
Hence the dynamical Einstein equations are satisfied.
Finally we have checked that all the 3+1 Einstein equations are satisfied by the $\delta=2$ Tomimatsu-Sato solution.