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3+1 Simon-Mars tensor in Kerr spacetime
This worksheet demonstrates a few capabilities of SageManifolds (version 0.7) in computations regarding 3+1 slicing of Kerr spacetime. In particular, it implements the computation of the 3+1 decomposition of the Simon-Mars tensor as given in the article arXiv:1412.6542.
The worksheet 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.
Spacelike hypersurface
We consider some hypersurface $\Sigma$ of a spacelike foliation $(\Sigma_t)_{t\in\mathbb{R}}$ of Kerr spacetime; we declare $\Sigma_t$ as a 3-dimensional manifold:
The two Kerr parameters:
Riemannian metric on $\Sigma$
The variables introduced so far satisfy the following assumptions:
Without any loss of generality (for $m\not =0$), we may set $m=1$:
On the hypersurface $\Sigma$, we are using coordinates $(r,y,\phi)$ that are related to the standard Boyer-Lindquist coordinates $(r,\theta,\phi)$ by $y=\cos\theta$:
Riemannian metric on $\Sigma$
The variables introduced so far obey the following assumptions:
Some shortcut notations:
The metric $h$ induced by the spacetime metric $g$ on $\Sigma$:
A matrix view of the components w.r.t. coordinates $(r,y,\phi)$:
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:
Check (comparison with known formulas):
For now on, we use the expressions Krp and Kyp above for $K_{r\phi}$ and $K_{ry}$, respectively:
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 $R = \gamma^{ij} R_{ij}$:
Test: 3+1 Einstein equations
Let us check that the vacuum 3+1 Einstein equations are satisfied.
We start by the contraint equations:
Hamiltonian constraint
Let us first evaluate the term $K_{ij} K^{ij}$:
The vacuum Hamiltonian constraint equation is \[R + K^2 -K_{ij} K^{ij} = 0 \]
Momentum constraint
In vaccum, the momentum constraint is \[ D_j K^j_{\ \, i} - D_i K = 0 \]
Dynamical Einstein equations
Let us first evaluate the symmetric bilinear form $k_{ij} := K_{ik} K^k_{\ \, j}$:
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, we have checked that all the vacuum 3+1 Einstein equations are fulfilled.
Electric and magnetic parts of the Weyl tensor
The electric part is the bilinear form $E$ given by \[ E_{ij} = R_{ij} + K K_{ij} - K_{ik} K^k_{\ \, j} \]
The magnetic part is the bilinear form $B$ defined by \[ B_{ij} = \epsilon^k_{\ \, l i} D_k K^l_{\ \, j}, \]
where $\epsilon^k_{\ \, l i}$ are the components of the type-(1,2) tensor $\epsilon^\sharp$, related to the Levi-Civita alternating tensor $\epsilon$ associated with $\gamma$ by $\epsilon^k_{\ \, l i} = \gamma^{km} \epsilon_{m l i}$. In SageManifolds, $\epsilon$ is obtained by the command volume_form() and $\epsilon^\sharp$ by the command volume_form(1) (1 = 1 index raised):
Let us check that $B$ is symmetric:
Accordingly, we set
3+1 decomposition of the Simon-Mars tensor
We follow the computation presented in arXiv:1412.6542. We start by the tensor $E^\sharp$ of components $E^i_ {\ \, j}$:
Tensor $B^\sharp$ of components $B^i_{\ \, j}$:
1-form $\beta^\flat$ of components $\beta_i$ and its exterior derivative:
Scalar square of shift $\beta_i \beta^i$:
Scalar $Y = E(\beta,\beta) = E_{ij} \beta^i \beta^j$:
Scalar $\bar Y = B(\beta,\beta) = B_{ij}\beta^i \beta^j$:
1-form of components $Eb_i = E_{ij} \beta^j$:
Vector field of components $Eub^i = E^i_{\ \, j} \beta^j$:
1-form of components $Bb_i = B_{ij} \beta^j$:
Vector field of components $Bub^i = B^i_{\ \, j} \beta^j$:
Vector field of components $Kub^i = K^i_{\ \, j} \beta^j$:
3+1 decomposition of the real part of the Simon-Mars tensor
We follow Eqs. (77)-(80) of arXiv:1412.6542:
Hence all the tensors $S^1$, $S^2$, $S^3$ and $S^4$ involved in the 3+1 decomposition of the real part of the Simon-Mars are zero, as they should since the Simon-Mars tensor vanishes identically for the Kerr spacetime.
3+1 decomposition of the imaginary part of the Simon-Mars tensor
We follow Eqs. (82)-(85) of arXiv:1412.6542.
Hence all the tensors ${\bar S}^1$, ${\bar S}^2$, ${\bar S}^3$ and ${\bar S}^4$ involved in the 3+1 decomposition of the imaginary part of the Simon-Mars are zero, as they should since the Simon-Mars tensor vanishes identically for the Kerr spacetime.