Rotating gravity

AstroNuclPhysics ® Nuclear Physics - Astrophysics - Cosmology - Philosophy Gravity, black holes and physics

Chapter 3
GEOMETRY AND TOPOLOGY OF SPACE-TIME
3.1. Geometric-topological properties of spacetime
3.2. Minkowski planar spacetime and asymptotic structure
3.3. Cauchy's role, causality and horizons
3.4. Schwarzschild geometry
3.5. Reissner-Nordström geometry
3.6. Kerr and Kerr-Newman geometry
3.7. Spatio-temporal singularities
3.8. Hawking's and Penrose's theorems on singularities
3.9. Naked singularities and the principle of "cosmic censorship"

3.6. Kerr and Kerr-Newman geometry

If the body that is the source of the gravitational field rotates , the excited external gravitational field will no longer be centrally symmetrical, but can only be axially symmetrical (if the mass-energy distribution in the rotating body is symmetrical with respect to the axis of rotation). In §2.5, passage " Rotating gravity " , we derived in the approximation of the weak field the effect of the rotation of a gravitational body on the external excited gravitational field. We have seen that the rotation of the source leaves characteristic "traces" in the form of non-diagonal members on the external gravitational field (ie on the space-time metric) , causing the outer bodies to be entrained by the rotating gravitational field in the direction of the source rotation.(so-called Lense-Thirring effect ) .
  The exact solution of Einstein's equations (in vacuum) for such an axially symmetric case was found by R. Kerr [152] in 1963; this solution was then generalized by E. Newman to the case of the presence of an electric charge [186]. 

Kerr geometry
Kerr geometry is a generalization of Schwarzschild geometry roughly in the sense that Schwarzschild geometry is "spherical", while Kerr geometry is generally elliptical . In the so-called Boyer-Lindquist coordinates (which are an elliptical generalization of Schwarzschild coordinates) [28], the space-time element of Kerr's geometry has the form

(3.37)

where M is the total mass (weight parameter) and a = J / M is "specific momentum" - total rotational angular momentum J divided by the total mass M . From the expression for the space-time element (3.37) it is clear (and this is confirmed by the calculation of the components of the curvature tensor R i klm and its scalar invariant) that Kerr's geometry has a physical singularity given by the relation
 

r 2 + a 2 cos 2 J   = 0.      

This is not a singularity point as in the Schwarzschild solution, but the ring singularity , which is in a plane perpendicular to the axis of rotation of the shape of a circle with radius a .

Similarly as in Reissner-Nordströmovì geometry are distinguished here three special cases of differing global space-geometrical structure: a 2 <M 2 , a 2 = M 2 , a 2 > M 2. Kerr geometry is of particular importance for the case M 2 > a 2 , where it describes the external field of stationary rotating objects , especially black holes. *). When R. Kerr derived the solution [152], he certainly had no idea how this "algebraically special" solution would prove important and general; in light of Theorem 4.1, a "black hole has no hair", any stationary uncharged black hole will have a Kerr geometry of spacetime.
*) This is exactly true for a black hole, where Kerr's geometry is a vacuum solution of Einstein's equations. However, finding a material source of exact Kerr geometry, leading according to Einstein's equations to a smooth transition of the inner metric to the outer Kerr metric, is by no means easy. The shape of such an ellipsoidal rotating source and the distribution of matter in it must satisfy certain very special conditions [82]. The gravitational field around the rotating material bodies (planets, stars, galaxies) is therefore only approximately Kerr.
  In most important case a 2 <M 2 there are two values of r , for which in the denominator of the spatial part of the metric v (3.37) r 2 -2Mr + a 2 is equal to zero:

r g +   = M + Ö (M 2 - a 2 ), r g -   = M - Ö (M 2 - a 2 ) . (3.38)

Thus, again (similarly to Reissner-Nordström geometry) there are two horizons - the outer horizon of events r = r g + and the inner horizon r = r g - (which is the Cauchy horizon), on which the metric (3.37) is pseudosingular. To reach the horizon, each object needs an infinitely long coordinate time (but a finite interval of its own time) and also an infinite angle ( j ®¥ ) - due to the entrainment of inertial systems by angular momentum (see §4.4) it must make infinitely many orbits around the horizon.
  To remove this coordinate pseudosingularity ( ie to analytically extend the metric across these areas) the transition to Kerr coordinates [127], [41] (v + , r, J , j ~ + ) is used by transformations

dv+ = dt + [(r2+a2)/(r2-2Mr+a2)].dr , dj~+ = dj + [a/(r2-2Mr+a2)].dr . (3.39)

This transformation performs an infinite "compression" of the coordinate time t and an infinite "twisting" of the angular coordinate j around the horizon. The metric (3.37) then has the form in Kerr coordinates

(3.40)

which is already analytical to r = r g + and r = r g - . The complete analytical extension is obtained by combining this metric in coordinates (v + , r, J , j ~ + ) and analogous metrics in coordinates (v - , r, J , j ~ - ) given by transformations
dv
- = dt - [( r 2 + a 2 ) / (r-2Mr + a)] .dr, d j ~ - = d j - [a / (r 2 -2Mr + a 2 )] .dr .

A conformal spacetime diagram of this complete extension of Kerr geometry is shown in Fig. 3.25a. The global structure here is similar to the structure of the Reissner-Nordström spacetime (compare with Fig. 3.21 in the previous §3.5 ) *), but the nature of the real singularity r = 0 is somewhat different. It turns out that in Kerr space-time this singularity has an annular structure and it is possible to extrapolate the geometry through it to negative values of the radial coordinate r [43], [28].
*) Here, too, there is an infinite number of "universes" between which it is possible to theoretically (model) "travel". A critical assessment of similar possibilities will be in §4.4, section " Black holes - bridges to other universes? ".


Fig.3.25. Conformal spacetime diagram of the complete extension of Kerr
geometry along the axis of symmetry.
a) Case M 2 > a 2 > 0. b ) Case M 2 = a 2 (extreme Kerr geometry). c ) Case a 2 > M 2 (Kerr's naked singularity).

In the case of M 2 = a 2 , r g + = r g - = M, the inner and outer horizons merge together. The full extension of this metric shown in Fig. 3.25b again has a similar structure to the Reissner-Nordström geometry at M 2 = Q 2, with the difference that analytical extension through the ring singularity to negative r is possible . The Kerr metric in this case describes the spacetime geometry of the extreme Kerr black hole with the maximum possible rotation speed (§4.4).
For a
2 > M 2 , the metric (3.37) is singular only for r = 0, which is  true singularity with an annular structure. Through the interior of this annular singularity, the solution can be analytically extended to negative values of r (Fig. 3.25c). There is no horizon and the singularity can therefore both "communicate" with the whole surrounding spacetime - it is Kerr's naked singularity (see §3.9 and §4.4).

Kerr - Newman geometry
We get another generalization if we consider the presence of an axially symmetric electromagnetic field, ie a rotating axially symmetric source will have an electric charge , which is also axially symmetrically distributed. The geometry of spacetime around such an object is called Kerr-Newman geometry [186]; it is in fact a combined Kerr and Reissner-Nordström geometry. The space-time interval element (in Boyer-Lindquist coordinates) has the form

(3.41)

where Q is the total electric charge measured by a distant observer - either by the flux of the electric intensity vector E through the closed surface, or by analysis of the trajectories of the charged test particles. As with Kerr's solution, the geometry of spacetime is stationary and axially symmetric . The outer horizon r = r g + (event horizon) and the inner horizon r = r g - (Cauchy horizon) have radii

(3.42)

Note: The event horizon r =r g + is also sometimes referred to as the Killing horizon , because the Killing vector field x o º¶/t (introduced in §2.4), its time component, here changes the space-time characteristic: outside the horizon it is of the time type while within the horizon it acquires a spatial character.

The global geometric structure of Kerr-Newman spacetime is analogous to the Kerr geometry described above. There are again three special cases :
a
2 + Q 2 <M 2 ( black hole ),
a
2 + Q 2 = M 2 ( extreme Kerr-Newman geometry),
a
2 + Q 2 > M 2 ( naked singularity ).

Carter [43] showed that in the vicinity of an annular singularity there is a region in which g jj <0; here the axial Killing vector / ¶j acquires a temporal character, so that closed worldlines of the time type appear here (eg circle t = const, r = const, J = const). In these areas around the singularity, therefore, causality may be violated . The assessment of the physical significance of some aspects of the complete extension of the Kerr-Newman geometry for black holes is in the case of §4.4, for n singularity in §3.9. The great significance of Kerr-Newman geometry lies in the fact that it is the most general solution for stationary axially symmetric asymptotically planar spacetime which has an event horizon, ie  the most general solution describing a black hole - in the spirit of the "black hole has no hair theorem" , see §4.5 " The "black hole has no hair" theorem ".

The motion of test particles (generally charged) in general Kerr-Newman spacetime is significantly more complicated than in Schwarzschild geometry. Even in the special case, when the motion will take place only in the equatorial plane and we do not consider the electric charge, the trajectory of the test particle near the horizon (especially in the ergosphere, see §4.4) will decisively depend, among other things, on the momentum of the particle. or the opposite direction with respect to the momentum J - i.e. if the particle moves in the direction or against the direction of rotation of the Kerr field source.
  The movement of charged test particles due to the action of electromagnetic forces will generally no longer take place after geodesics; on the right side of the geodetic equation budLorentz force appears instead of zero:

(3.43)

where q is the electric charge of the test particle and F ik is the tensor of the electromagnetic field cooperating as the source of the given Kerr-Newman geometry.
 
Analysis of the motion of test particles in the Kerr-Newman field is mostly done not from the basic d of equation (3.43), but had equivalent using the Hamilton-Jacobi equations [165], [43] which is easier to determine the symmetry of the integrals of motion. The resulting equations of motion of a test particle with charge q, rest mass m o , energy E with respect to infinity, axial component of momentum L j and component p J of momentum were derived by Carter [43], [181]:

Since the gravitational and electromagnetic fields are stationary and axially symmetric (ie both components of the metric g ik and the four potential A k do not depend on t and j ), the following quantities will be constants (integrals) of motion when moving the test particle: energy E with respect to infinity, axial component L .. angular momentum with respect to the axis of symmetry, electric charge q of the particle and its rest mass m o (which at each point of the trajectory is related to the four-momentum of the particle by the relation m o = (- g ik p i p k ) 1/2). Another integral of motion that does not follow from the above symmetries was found by Carter [43]:

C = P J 2 + a 2 (m 2 - E 2 ) + (L j 2 / sin 2 J ) .cos 2 J   ; (3.45)

because we will not need this quantity in the next, we did not lead it into the equations of motion (3.44) .
  We will not perform a general analysis of particle motion in Kerr-Newman spacetime based on equations (3.44) here, the interested party can find details eg in [8], [81], [237]. However, we will use some of the consequences of equations (3.44) for the motion of particles in Kerr-Newman spacetime under §4.4 " Rotating and electrically charged Kerr-Newman black holes ", where we discuss the most physically important aspects of Kerr-Newman geometry (such as the effect entrainment of local local inertial systems, existence of ergosphere, Penrose process, superradiation, etc.) in connection with the properties of black holes.

Kerr-Newman geometry with nonlinear electrodynamics
At the end of the previous §3.5, devoted to Reissner-Nordström spacetime with centrally symmetric electric charge, we briefly mentioned the possibility of generalization for the case of
nonlinear electrodynamics - the passage " Reissner-Nordstrom solution with nonlinear electrodynamics ". An analogous generalization can be made for Kerr-Newman geometry. When using Born-Infeld nonlinear electrodynamics ( §1.6, passage " Nonlinear electrodynamics " ) with the parameter nonlinearity b in the space-time interval (3.41):

(3.41)

instead of a simple square of the charge " Q 2 " there will be more complex functions "f (r, Q)"

 

analogous to metric (3.36), containing elliptic integrals

 

where "F (...)" is the Legender's elliptic function of the 1st kind and " 2 F 1 (...)" is the so-called hypergeometric function (more complex power series from Q 2 b 2 / r 4 ) . .
  For this " Kerr-Newman-Born-Infeld " metric, due to the excessive computational complexity, it has not yet been possible to find a completely general analysis of the motion of the test particles. Trying to approximate solutions against slow rotation (a << 1), using methods perturbation analysis . ............ ............... 

3.5. Reissner-Nordström geometry   3.7. Spatio-temporal singularities

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Vojtech Ullmann