Wave Fronts in a Causality-Violating Gödel-Type Metric
The light rays and wave fronts in a linear class of the Gödel-type metric are examined to reveal the causality-violating features of the space-time. Noncausal features demonstrated by the development of unusual wave front singularities are shown to be related to the nonmonotonic advance of time along the light rays, as measured by a system of observers at rest with respect to one another with synchronized clocks.
In general relativity, local space-times have the same causal structure as flat, Minkowski space-times, because all space-times are locally Minkowskian. On the nonlocal scale, however, significant differences may arise as the field equations of general relativity do not provide nonlocal constraints on the underlying space-times. Indeed, it has long been known that there are solutions to Einstein’s field equations that present nonlocal causal anomalies in the form of closed time-like curves, closed null geodesics, and closed time-like geodesics.
The renowned model found by Gödel  is possibly the best known example of a solution to Einstein’s field equations, with a physically well-motivated source, possessing causal anomalies. The Gödel solution makes it apparent that general relativity permits solutions with closed time-like world-lines, even when the metric possesses a local Lorentzian character that ensures an inherited regular chronology and, therefore, the local validation of the causality principle.
This modern understanding of the Gödel metric has led to an increased interest in examining solutions to Einstein’s field equations with unusual topological features, all of which suggest a broad richness in possible theories of gravity. Solutions have examined closed time-like curves (see, e.g.,  and related references therein), closed null geodesics (e.g., ), and closed time-like geodesics (e.g.,  and related references therein) in space-times with unusual equations of state. Section 2 describes a range of classes of the Gödel-style metrics, including the one analyzed in more detail in this paper, and enumerates the current understanding of geodesics in those metrics.
To gain broader insight into these anomalies, we examine the properties of light rays and wave fronts of null geodesics emitted by point sources in a Gödel-type metric in this paper. The light rays and null wave fronts reveal some of the causality-violating features of the space-time, and we contrast the structure of these wave fronts with those in the Gödel space-time. These comparisons allow us to both discuss the nature of wave fronts as nonlocal phenomenon and discuss the causality-violating aspects that are possible. Because not much is known about the broad properties of these new Gödel-type metrics, this paper provides a unique window into some of their properties.
Section 2 discusses the variety of Gödel-type metrics possible in order to position the metric considered in this paper. In Section 3, we outline the equations for geodesics and discuss the meaning of the time variable which will be key in our understanding of wave fronts. Sections 4 and 5 present pictures of individual light rays and the wave fronts and discuss how these develop in time for rays in a plane of symmetry. A more thorough discussion of how wave front singularities, and other noncausal features, arise is discussed in Section 6. In Section 7, three-dimensional wave fronts are presented, followed by a final discussion and conclusion.
2. Characterization of a Linear Class of Gödel-Type Metrics
A particularly simple Type D metric has recently examined a member of a linear class of Gödel-type metrics . Previously, relativistic quantum motion of spin- particle without interactions , linear confinement of a scalar particle subject to a scalar and vector potentials of Coulomb-types , Dirac equation , spin- system of DKP equation , and DKP oscillator  was investigated in this Type D metric.
where and are constants and the prime denotes a derivative with respect to .
There are several different classes of Gödel-type space-time geometries, including a linear, trigonometric, or spherical and a hyperbolic class which we discuss below.
Case 1. Linear class: to obtain a linear class of Gödel-type metrics, one can take in the condition Equation (2). The Som-Raychaudhuri metric  and the solution given by Reboucas and Tiommo  are the examples of this class of solutions. In our case, the study space-time satisfies the condition Equation (2) with which clearly indicates that the metric we consider in this paper also belongs to this linear class metrics.
The Som-Raychaudhuri metric in polar coordinates is given by
The geodesic equations of motion in Gödel-type space-times have been analyzed by several authors. Numerous publications concerning the solutions to the geodesic equations of the Gödel universe and Som-Raychaudhuri space-time were known in the literature dating back at least to . The geodesic equations for the Gödel metric were firstly solved by Kundt  where the Killing vectors and corresponding constants of motion were used. Novello et al.  have studied a detailed discussion on the geodesic motion in the Gödel universe using the method of effective potential as well as the analytical solution. Pfarr  investigates both geodesic and nongeodesic motion of test particles in the Gödel universe. More recently, a very convenient set of coordinates, in which the Gödel universe reveals its properties more apparently, was discussed . There, the symmetries of the Gödel universe were provided, alongside a special solution to the geodesic equations. The understanding of null geodesics provides the bedrock for ray tracing in Gödel and Gödel-type space-time geometries. Egocentric visualizations of certain scenarios in the Gödel universe can be found in Grave and Buser . There, the authors presented much more improvements for visualization techniques regarding general relativity. Furthermore, finite isometric transformations were used to visualize illuminated objects. This method was technically reworked and improved in  and resulted in an interactive method for visualizing various aspects of the Gödel universe from an egocentric perspective. There, an analytical solution to the geodesic equations and a numerical integration of the equations of isometric transport were used. The analytical solution of the geodesic equations of Gödel’s universe for both particles and light in a special set of coordinates which reveals the physical properties of this space-time in a very transparent way was studied in . They also recapitulate the equations of isometric transport for points and derive the solution for Gödel’s universe. The Gödel universe through world-lines associated with motion at constant speed and constant acceleration orthogonal to the instantaneous velocity (WSAs) was studied in . They have shown that these world-lines can be used to access every region—both spatial and temporal—of the space-time.
The approaches of previous authors, in particular Paiva et al.  to solving for individual geodesics are similar to the results of this paper. The current study differs by considering families of null geodesics, emitted at one space-time point in all spatial directions, and organizing the points along the geodesics according to a time foliation consistent with the observations of the observer who emitted the light pulse. The global structure of the null geodesic wave fronts organized in this fashion shed a different perspective on the time anomalies described in the literature when looking at individual geodesics.
3. Geodesics for Observers and Light Rays
In this paper, we analyze a particular Gödel-type space-time of Type D metric, a linear or flat class of Gödel-type solutions . This metric is given by (see also, Refs. [6–9]) where is a real parameter and the Cartesian coordinates extend from minus to plus infinity.
Based on the metric as presented in Equation (4), we introduce a Lagrangian defined by where represents a derivative with respect to an affine parameter . Because , , and do not appear in the Lagrangian, we have three types of conserved momentum, , and . This means that the Euler-Lagrange equations will result in one second-order and three first-order ordinary differential equations for geodesics.
3.1. Geodesic Equations
The Euler-Lagrange equations for and are trivially coupled:
In the Euler-Lagrange equation, we choose the constant as so that at an initial condition where , positive values correspond with positive . Equation (8) can be trivially decoupled, resulting in
For the coordinate, the Euler-Lagrange equation results in
but we can substitute our results for and and simplify the result to obtain
Equation (12) is the equation for a simple harmonic oscillator with an offset to the central position from the origin. Defining
and substituting into Equation (12) results in
so that the solution for is given by
With this solution for , we can solve for by simply substituting into Equation (10), with the result
The equation for is trivially
A similar substitution procedure results in an analytic expression for , even though this expression is not simple.
For convenience and future reference, we note that the solutions for the spatial part of the geodesics and the velocities associated with these coordinates is given by
3.2. Boundary Conditions for Static Observers
In this paper, we wish to examine the wave fronts of null geodesics. Wave fronts are fundamentally nonlocal constructions, particularly wave fronts of constant time. An observer must reconstruct the wave front based on information from observers distributed throughout the space, who all, ideally, have synchronized clocks.
From the metric, we notice that an observer at rest in the space-time would carry a clock which reads the proper time. The question is whether an observer at the origin can work with a team of observers who remain at rest relative to her. If so, then a system of synchronized clocks reading the proper time can be constructed, and a wave front of constant time is a physically realizable nonlocal construct.
Our goal therefore is to show that there are time-like geodesics for which the observers hold their position at . This is trivial in the direction: . From Equation (10) we see that for at all , we need to fix the value of :
With this restriction on , we see that is zero at ,
Further, Equation (24) implies that the constant in equation is . Therefore, with the restriction on given in Equation (24) with , we see that it is simply possible to set in Equation (23) with . The result is that the geodesic maintains the position with no velocity or acceleration.
3.3. Boundary Conditions for Null Geodesic Wave Fronts
To consider wave fronts of null geodesics, we would now like to consider the boundary conditions to be of the form that at , the light rays are at the origin (with ) with initial velocities given by . We see that this can be accomplished by setting
In this case, we now have
We are free at this point to set . Then, rearranging the restriction that the geodesics are light rays results in
so that we see that is restricted in the range . Introducing a parameter , we take
The meaning of is that for a light ray in the plane, is the angle the initial light ray velocity makes with the axis. With these definitions, a choice of and then fixes a particular light ray emanating from the origin.
A wave front of null geodesics is a two-parameter family of light rays. We construct this wave front by allowing the parameters to run through all their allowed values, with the additional requirement of taking one set of values with the positive sign in both equations in (33) and one set of values with one positive and one negative sign.
3.4. Time along Null Geodesics
With the definitions for in Equation (29) and in Equation (9), we can explicitly integrate to obtain a function for with a boundary condition that at . The result is rather long and complicated, but critically, it is largely dominated by a linear term in with “wiggles.” The resulting time along null geodesics parametrized by with is
4. Individual Light Rays
We begin by considering individual light rays in the plane found by setting . All such light rays form closed loops in the plane.
Figure 1 shows four light rays with varying values of for Equation (29) and . We see that all rays form spatially closed loops that extend out to a maximum radius of . We therefore will interpret the circle of radius as the spatial part of a causal boundary beyond which an observer at the origin cannot communicate with directly.
These spatially closed light ray paths have complicated development in time. We note that the coordinate represents the proper time of all observers who maintain a fixed position, and in particular, it is the proper time of a freely falling observer at the origin. As we have seen, it is possible to form a system of freely falling observers at rest with respect to one another such that the proper time of all these observers is a set of synchronized clocks.
All light rays trace out circular paths that progress consistently in one direction (counterclockwise) in terms of the affine parameter . However, the behavior of light rays in terms of the time coordinate is more complicated. For rays with , the advancement of the time coordinate monotonically increases with the affine parameter. However, for larger , the time coordinate as a function of the affine parameter undergoes reversing periods where increases in affine parameter lead to decreases in the time.
This means that if an observer at the origin flashed a light in a particular direction, it would trace a closed loop path through the space, but also that our system of observers at rest in the space-time would consider the light path to not circle around uniformly in time. Rather, according to this system of observers, at a later time, a pair of light pulses spontaneously appear (out of the blue sky) at a point along this closed loop traveling in both directions along the loop as shown in Figure 1. The part of the blue sky pulse propagating with the original direction returns to the observer at the origin, while the portion of the pulse propagating in the other direction runs into the original pulse from the origin and the pair vanish. Put another way, for some stationary observers, the light ray would appear to be traveling in the “opposite” direction from its propagation with respect to the affine parameter.
By comparison, the situation in the Gödel metric for light rays in the azimuthal plane has some similarities and some striking differences. Light rays that are emitted from the origin in the Gödel space-time also form closed spatial loops in the azimuthal plane, with a distinct circular boundary that is taken as separating causal regions. However, for all such light rays emitted from the origin in the Gödel space-time, the time coordinate increases monotonically with the affine parameter.
However, when considering light rays emitted from a point , away from the origin in the Gödel space-time, the time coordinate does not increase monotonically. These rays do, however, cross over the circle that represents the causal boundary for an observer at the origin. Similar to the case in the Type D metric, the mathematics indicates that the observer at the origin would consider the pulse emitted at to undergo the same type of behavior as described above, as is shown in Figure 2. However, both the blue sky appearance and the annihilation of the pulse pairs occur outside the causal boundary for an observer at the origin, hiding much of the odd behavior .
5. Wave Fronts in the Plane
In this section, we begin to examine wave fronts of null geodesics emitted from a point source at the origin. As each null geodesic advances in its affine parameter, it moves through the space as well as through time. Our perspective is that an observer remaining stationary at the origin has emitted a pulse of light in all directions simultaneously. We will consider points from different null geodesics to belong to the same wave front if they have the same coordinate—the proper time of the system of observers who remain at rest relative to the observer who released the light pulse at the origin.
Because of conservation of momentum in the direction, many of the key features of the wave fronts in Gödel-type metrics can be understood from the advances of wave fronts in the plane. In the case of a Gödel metric, all the null geodesics emitted by an observer at the origin rebound off a circle that separates the causal region. Figure 3 shows points along the wave fronts in the Gödel metric, which are rotating circles.
In the metric considered in this paper, the situation is significantly different, due to the time reversals revealed in Section 4. Figure 4 shows the wave front at eight consecutive times for a pulse of light emitted at the origin. Due to the nonmonotonic nature of the time coordinate along the null geodesics, wave fronts of constant time show “blue sky”-style bifurcations in the plane where a portion of the wave front appears out of nowhere and attaches to the main wave front. Later, a new section breaks off and disappears. The entire wave front is rotating counterclockwise.
Clear cusps appear on the wave front as well. Cusps are a standard form of wave front singularity. We will see in the next section how these cusps arise as folds in the time cut functions of the light cone.
The situation for wave fronts from the origin in the Type D metric is similar to that of the Gödel metric for wave fronts of constant time constructed by an observer at the origin when the initial pulse of light is emitted away from the origin. Figure 5 shows the advancing wave front of constant time of a pulse of light in the plane when the initial location of the pulse is away from the origin. In this case, there are again blue sky bifurcations where portions of the wave front appear, then connect to the main portion, then break free and disappear.
The principle difference between the wave fronts of constant time from points at the origin in the Type D metric and from points away from origin in the Gödel metric is that the blue sky bifurcations in the Gödel metric appear outside the circle that is the horizon for the observer at the origin. This means that the observer at the origin who is reconstructing the wave fronts using her time coordinate will never see or communicate with observers who saw disconnected portions of the wave front. By contrast, the observer at the origin in the Type D metric would communicate with observers who indicate the presence of the portion of the wave front formed from the blue sky bifurcations.
6. Time, Light Cones, and Wave Fronts
As opposed to the constant time wave fronts, the light cones in the metric considered in this paper are very simple. Figure 6 shows future light rays with plotting the motion in the plane against the affine parameter on the vertical axis. The light cone with the components suppressed is simply a rotating series of light rays that rebound off the limiting circle of radius .
The time coordinate along the light cone, however, is a complicated function. Figure 7 shows a series of reference light rays comprising the light cone and a large number of points along light rays when —which is a time where cusps have formed after a blue sky bifurcation in the time wave front—as we see in Figure 4. This time cut folds over itself revealing cusp singularities as one sees in the canonical case presented in Arnol’d .
Figure 8 shows three time cuts: at as a small closed loop near the base of the light cone; at which is a slightly larger loop, but also two separate side loops that have grown from blue sky bifurcations along the sides of the light cone; and finally, at where the separate time cuts have rejoined the main group, but in a way that leads to overlaps that project into the plane with caustics. This is made explicit in Figure 9 which shows the exact same light cone and three time cuts as Figure 10 but from directly above the light cone so that one sees the projection of the time cuts into the plane.
7. Wave Fronts in Three Dimensions
The three-dimensional wave fronts of the Type D metric considered in this paper reveal how the caustic structures in the two-dimensional cases arise. Figure 11 shows a series of six constant time wave fronts in three spatial dimensions for . Each plot is shown from the same vantage point with the direction oriented out of the page and towards the right, the direction oriented towards the top of the page, and the direction oriented out of the page and towards the left. The three-dimensional wave fronts begin as a topological sphere centered at the origin but slowly distort along an axis in the plane.
At , we see that a pair of blue sky bifurcations has developed in two areas. We see in Figure 12 that these blue sky sections have a three-dimensional structure with circular cusp ridge that bounds two smooth connecting surfaces. The blue sky bifurcation sections connect shortly after with the main wave front with two cusp ridges along the outside edge. These parts of the wave front correspond to light rays being observed as in three spatial positions at a given time beginning at point , as in Figure 2.
Between roughly and , the wave front maintains a cusp ridge that rotates and begins to align with the axis. Near , the wave front begins to collapse on itself as is shown in Figure 13. In two regions symmetric with the axis, the wave front comes together, and when the contact occurs, holes in the wave front become apparent as is shown in Figure 11 at . Those holes quickly grow, and eventually, the wave front breaks apart leaving a central tube, surrounding the axis as it collapses, and two spear- or hook-like structures with cusp ridges that are advancing parallel to the axis. The breaking apart of the wave front in three dimensions results in the blue sky vanishing of a portion of the wave front in the plane in Figure 5. These portions of the wave front are created when light rays which had three spatial positions at the same coordinate time according to our system of observers recombine at point in Figure 2.
The process continues as the light rays with new light rays undergoing time reversals. In Figure 14, we see that at , a new disconnected region of the wave front appears. These sections combine with the main body of the wave front as in Figure 15, and then the body rotates as before, develops two pinch points, and begins to open up. After the opening breaks apart, a new set of spear-like sections appears, as is shown in Figure 16. A small cusp ridge remains on each end of the progressing wave front as a remnant of the previous spear structure.
Wave fronts of light rays are fundamentally nonlocal reconstructions of a causal feature of any space-time. The light cone itself is the central structure of causality; it separates regions of causal contact, and properties in the light cone structure control communication between points in the space-time. As we see in Figure 6, the light cones in the space-time we study here are contained to a nonlocal region of the space-time but are not global structures extending throughout the entire space-time.
How one chooses to slice a light cone is not necessarily inherently obvious in a given space-time. In some space-times, there may arise a natural system of observers who share some common notion of time. For example, in the Friedman-Robertson-Walker (FRW) cosmological metrics, there is a natural, or preferred, frame of reference in which all the matter is homogeneous and isotropic, and this frame can be extended across the entire space-time. Therefore, in FRW metrics, or metrics that are approximately FRW such as those considered in standard gravitational lensing studies, there is a natural slicing to the light cone associated with the clocks of observers at rest with respect to the cosmic flow.
On the other hand, in asymptotically flat space-times such as the Kerr-Newman metrics, there is not one system of observers following freely falling, or geodesic, trajectories that share a common synchronized clock system. Even though these black-hole space-times are very physically motivated, general relativity does not permit a single global coordinate system of synchronized clocks with which to slice the light cones. The best one could do is to consider wave fronts of constant coordinate time, taking this time to physically mean the clock time of an observer in the asymptotically flat limit.
In Section 3.2, we show that although the “natural” motion in the Type D metric considered in this paper is rotational, there is a family of observers who follow geodesic motions and remain at rest with respect to one another. This family shares a common notion of time, and it is with respect to this system of observers that we have drawn our constant time wave fronts. We note that a similar set of observers can be constructed in the Gödel metric, though we do not show this result in this paper.
This result is surprising, as prior literature shows that there are no global surfaces of simultaneity in the Som-Raychaudhuri space-times. Section 3.2 shows that in the particular metric examined in this paper, there is a set of geodetic observers who extend throughout the space-time region containing the light cone, who remain at rest with respect to one another, and who share a common notion of time. In terms of these observers, who extend across a finite but nonlocal region, we plot wave fronts of constant time.
In the case of FRW metrics, null geodesic wave fronts emanating from a point source maintain spherical shapes. While the wave fronts will remain spheres, the radius of those spheres as a function of the cosmic time coordinate does depend on both the expansion of the universe and the nature of space, for instance, whether the universe is closed. However, the wave front does not develop singularities, except possibly point-like singularities associated with the light traveling fully around a closed universe should that be possible before a big crunch. Likewise, the wave front does not develop nonconnected features, because while the light cones in FRW metrics might lead to particle horizons, there are no noncausal time features in the FRW metrics.
In this paper, we have shown that a central observer can organize and directly communicate with a system of observers who follow geodesic motion, share synchronized clocks, and are at rest with respect to one another. When this central observer emits pulses of light in all directions, and reconstructs the wave fronts from her direct communication with a system of observers, nonconnected wave fronts and unusual wave front singularities are observed.
The presence of nonconnected regions in constant time wave fronts of light rays in the Type D metric considered in this paper is evidence of the strongly noncausal features of the space-time. The fact that the wave fronts are not simply connected helps to demonstrate the notion that there is no globally defined surface of simultaneity. We strongly suspect that in a space-time where there is a globally defined surface of simultaneity, it would not be possible to see nonconnected regions in the constant time wave fronts of null geodesics.
Interestingly, in the Gödel space-time, a similar set of observers (at rest with respect to the central observer, in direct communication, using a common sense of time) does not record noncausal features of the wave fronts from pulses of light emitted by the central observer. For light emitted from the central position, no noncausal wave front singularities are observed.
This paper examines wave front singularities in a Gödel-type Type D metric. The wave fronts demonstrate several interesting noncausal features of the metric, and the analysis of the metric and wave front brings to light interesting issues related to the study of wave fronts in gravitational lensing and the study of causal metric spaces.
In terms of gravitational lensing, the spatial location of wave front singularities in the light cone of an observer is a location where significant magnification of sources of light appears. In this paper, we see typical wave front singularities (such as the cusp ridge), as well as atypical features. To our knowledge, the appearance of disconnected portions of the constant time wave fronts in regions where the observer receives light rays directly is unusual. It does not, for instance, happen in the Gödel metric.
The relation between the light cones and the wave fronts is also of interest. The development of the light cones is smooth and consistent in terms of the affine parameter. Figure 9 shows two examples of the formation of wave front singularities outlined in the literature, for instance, in Arnol’d . First, in the connected portion at , we see that the time cut of the light cone is in one smooth portion along what Arnol’d calls the big wave front in space that includes the affine parameter but that the projection of this cut into the space has cusps. Second, we see an unusual feature of wave front singularities—that a disconnected portion of the wave front can be born away from the main section if the constant time cut of the light cone is not connected.
The appearance of this second form of null-geodesic wave front singularity distinguishes the Gödel-type metric examined in this paper from the usual Gödel metric. These features indicate a broader class of causal behavior than is typically seen, and the results of this paper further the understanding of the range of possible behavior permitted by general relativity, at least mathematically.
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Conflicts of Interest
Authors declare that there are no conflicts of interest regarding publication this paper.
ML acknowledges the financial support of Bridgewater State University through a Summer Grant from the Adrian Tinsley Program for Undergraduate Research. The three-dimensional wave front plots were created using the Walnut package created by Eric Grotzke. Light ray and wave front diagrams for the Gödel space-time were originally reported in a paper by Kling et al. .
V. I. Arnol’d, Catastrophe Theory, Springer-Verlag Berlin Heidelberg, Berlin, Heidelberg, 1992.View at: Publisher Site