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Path: blob/master/sage/SageManifolds/SM_Tomimatsu-Sato_3p1.sagews
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3+1 Einstein equations in the Tomimatsu-Sato spacetime
This worksheet is based on SageManifolds (version 0.7) and regards the 3+1 slicing of the 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 of a larger family of solutions parametrized by a positive integer and exhibited by Tomimatsu and Sato in 1973 [Prog. Theor. Phys. 50, 95 (1973)], the member 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.
Spacelike hypersurface
We consider some hypersurface of a spacelike foliation of Tomimatsu-Sato spacetime; we declare as a 3-dimensional manifold:
On , we consider the prolate spheroidal coordinates , with , and :
Riemannian metric on
The Tomimatsu-Sato metric depens on three parameters: the integer , the real number , and the total mass :
We set and choose a specific value for :
Furthermore, without any loss of generality, we may set (this simply fixes some length scale):
The parameter is related to by :
Some shortcut notations:
The Riemannian metric induced by the spacetime metric on :
A matrix view of the components w.r.t. coordinates :
Lapse function and shift vector
Extrinsic curvature of
We use the formula which is valid for any stationary spacetime:
The component :
The type-(1,1) tensor of components :
We may check that the hypersurface is maximal, i.e. that :
Connection and curvature
Let us call the Levi-Civita connection associated with :
The Ricci tensor associated with :
The scalar curvature :
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 :
The vacuum Hamiltonian constraint equation is
In vacuum and for stationary spacetimes, the dynamical Einstein equations are
Hence the dynamical Einstein equations are satisfied.
Finally we have checked that all the 3+1 Einstein equations are satisfied by the Tomimatsu-Sato solution.