A Central Mass in a Stationary Vacuum without Spherical or Axial Symmetry

A vacuumspacetimewith a centralmass is derived as a stationary solution to Einstein’s equations.The vacuummetric has a geodesic, shear-free, expanding, and twisting null congruence k and thus is algebraically special. The properties of the metric are calculated. In particular, it is shown that the spacetime has an event horizon inside which there is a black hole.Themetric is neither spherically nor axially symmetric. It is therefore in interesting contrast with the majority of metrics featuring a central mass which have one or more of these symmetry properties. The metric reduces to the Schwarzschild case when a certain parameter is set to zero.


Introduction
In this paper, we present a special solution of Einstein's equations which can be described as a stationary vacuum spacetime with a central mass singularity without spherical or axial symmetry.Apart from the mass , the metric will depend on a single parameter , and it reduces to the Schwarzschild solution when  is set to zero.
The character of this spacetime will be such that the Weyl tensor has a multiple null eigenvector  forming a geodesic, shear-free, and diverging twisting congruence.Thus, in terms of the Newman-Penrose spin coefficients, we can write as properties of  the following: Θ being the divergence and  the twist.Since the solution to be derived is vacuum, the previous properties mean that the metric will be algebraically special, so that of the Weyl complex coefficients we have Reference to the spacetime will be via a complex null tetrad , bar, , and  with labels 1, 2, 3, and 4, respectively, k being the vector described earlier.The field equations for a vacuum metric that admits a geodesic, shear-free, and diverging null congruence  were obtained by Kerr [1] and I. Robinson and J. R. Robinson [2] and further developed by Debney et al. [3].A different approach to obtaining vacuum solutions was made by Kinnersley [4].Here we follow mainly the methods of [5] and finally derive our solution in the specific form of (16).
Since the central mass will be without spherical or axial symmetry, in contrast with the well-known GR vacuum solutions with mass singularity, it is believed that the derived spacetime in its final form (16) is of significant interest.

Basic Equations
In relation to the null tetrad, we will employ coordinates   = , , , and  for  = 1, 2, 3, and 4, respectively.The spacelike coordinate  is complex,  being its conjugate,  an affine parameter along the  lines, and  a retarded time.We will use the notation of [5, chapters 29 and 30].The metric signature will be taken to be +2 and the speed of light and the Einstein gravitational constant to be unity.The spacetime metric, in terms of 1-forms relating the null tetrad to the   system, is [2,3,5] where In the   system, we then have Here, for the case of a stationary solution, The coefficient of  2 is −2, where Here , , and  are real functions and  a complex function, of  and . is a real function and  a complex function, of , , and . is a constant (>0).A subscripted comma indicates partial differentiation.For a stationary vacuum spacetime, the equations are where Calculations will be made in the tetrad frame whose metric coefficients are ] . (10)

A Stationary Vacuum Spacetime
We take  and  to be Referring to (7), we find that Calculation of the Riemann tensor showed that all components vanish when  → ∞.The metric is therefore flat at infinity.It was verified that  0 =  1 = 0, and in fact calculation leads to a Petrov type D. The vacuum equations (8) are evidently satisfied, and indeed all components of the Ricci tensor vanish confirming a vacuum metric.
For the curvature of the ,  2-surface, a function depending on  and  as well as  was obtained.It follows that the metric is neither spherically symmetric nor axisymmetric (see also Section 4).
From the Newman-Penrose spin coefficient , we obtain for the divergence and twist of the  lines respectively.

The Metric in Real Coordinates
If we make the transformation then the metric coefficients can be expressed in terms of real coordinates , , and , numbered 1, 2, and 3, respectively.Thus, the transformed metric coefficients   become We note that if we set  = 0, the metric reduces to the Schwarzschild spacetime (in Eddington-Finkelstein coordinates).In terms of these coordinates, the divergence and twist of the  lines, given by ( 14), have the expressions Also, it may be verified that the component   is the transform of −2 where  is given in (13).
The hypersurfaces  =  + and  =  − which satisfy the relation are null surfaces.They form horizons and they are real for In this case,  =  + is an event horizon and  will be spacelike in its exterior but timelike in the region  − <  <  + (where  will be spacelike).
From the metric, we see that a radial light ray ( =  =  = 0) which satisfies has / > 0 in the region  >  + , where 2 2 − 4 +  2 sin 2  cos 2  > 0. However, in the region  − <  <  + where the factor 2 2 − 4 +  2 sin 2  cos 2  < 0, we have / < 0, so that the light ray, and indeed all timelike particle motions, can only be inwards and never outwards.Thus, the metric has a black hole if 0 <  < √ 2.Setting  = 0, we get the familiar results for the black hole in the Schwarzschild solution.
We may verify in these coordinates that the Riemannian curvature of the ,  2-space ( = const;  = const) depends on  and  as well as , so that the metric is not spherically symmetric or axially symmetric.For the curvature, we derive When  = 0, this result becomes 2/ 3 , as appropriate to the Schwarzschild spacetime.The only Killing vector, when  ̸ = 0, is   reflecting the stationary character of the solution.

Conclusion
In this paper, we have derived and described the properties of a stationary vacuum metric which has no spatial symmetry but reduces to the Schwarzschild spacetime when the parameter  is set to zero.The spacetime is algebraically special and possesses a null congruence  which is geodesic, shear-free, and whose divergence and twist are calculated.Subject to the relation 0 <  < √ 2, there is shown to be an event horizon inside which there is a black hole.These features are believed to be of critical interest since they are in contrast with most previous discussions which have concerned a central mass in a spherically or axially symmetric environment.