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Path: blob/master/sage/SageManifolds/SM_Kerr_Newman.sagews
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Kerr-Newman spacetime
This worksheet demonstrates a few capabilities of SageManifolds (version 0.8) in computations regarding Kerr-Newman spacetime, especially the check of Maxwell equations and Einstein equations.
It is released under the GNU General Public License version 3.
(c) Eric Gourgoulhon, Michal Bejger (2015)
The corresponding worksheet file can be downloaded from here.
Spacetime manifold
We start by declaring the Kerr-Newman spacetime as a 4-dimensional diffentiable manifold:
Let us use the standard Boyer-Lindquist coordinates on it, by first introducing the part covered by these coordinates
Metric tensor
The 3 parameters , and of the Kerr-Newman spacetime are declared as symbolic variables:
Let us introduce the spacetime metric:
The metric is defined by its components in the coordinate frame associated with Boyer-Lindquist coordinates, which is the current manifold's default frame:
The lapse function:
Electromagnetic field tensor
Let us first introduce the 1-form basis associated with Boyer-Lindquist coordinates:
The electromagnetic field tensor is formed as [cf. e.g. Eq. (33.5) of Misner, Thorne & Wheeler (1973)]
The Hodge dual of :
Maxwell equations
Let us check that obeys the two (source-free) Maxwell equations:
Levi-Civita Connection
The Levi-Civita connection associated with :
Let us verify that the covariant derivative of with respect to vanishes identically:
The nonzero Christoffel symbols (skipping those that can be deduced by symmetry of the last two indices):
Killing vectors
The default vector frame on the spacetime manifold is the coordinate basis associated with Boyer-Lindquist coordinates:
Let us consider the first vector field of this frame:
The 1-form associated to it by metric duality is
Its covariant derivative is
Let us check that the vector field obeys Killing equation:
Similarly, let us check that is a Killing vector:
Another way to check that and are Killing vectors is the vanishing of the Lie derivative of the metric tensor along them:
Curvature
The Ricci tensor associated with :
Let us check that in the Kerr case, i.e. when , the Ricci tensor is zero:
The Riemann curvature tensor associated with :
The component of the Riemann tensor is
The expression in the uncharged limit (Kerr spacetime) is
while in the non-rotating limit (Reissner-Nordström spacetime), it is
In the Schwarzschild limit, it reduces to
Obviously, it vanishes in the flat space limit:
Bianchi identity
Let us check the Bianchi identity :
If the last sign in the Bianchi identity is changed to minus, the identity does no longer hold:
Ricci scalar
The Ricci scalar of the Kerr-Newman spacetime vanishes identically:
Einstein equation
The Einstein tensor is
Since the Ricci scalar is zero, the Einstein tensor reduces to the Ricci tensor:
The invariant of the electromagnetic field:
The energy-momentum tensor of the electromagnetic field:
Check of the Einstein equation:
Kretschmann scalar
The tensor , of components :
The tensor , of components :
The Kretschmann scalar :
A variant of this expression can be obtained by invoking the factor() method:
As a check, we can compare Kr to the formula given by R. Conn Henry, Astrophys. J. 535, 350 (2000):
The Schwarzschild value of the Kretschmann scalar is recovered by setting and :