2. Anisotropy of the Schwarzschild Metric
The Schwarzschild metric has the following form:
The exterior metric, which describes the spacetime around a spherically symmetric mass is given for values of where u is the Schwarzschild radius related to the mass M of the source given by . This metric treats the mass of the source as being concentrated at point at the center of the spacetime.
So if we have a spherically symmetric distribution of mass in some region, we can model the vacuum outside that region using the exterior Schwarzschild metric with an where M is the total mass contained in the region in question. So the vacuum surrounding any finite, static, spherically symmetric volume of mass can be described using the exterior Schwarzschild metric, and the mass is treated as a Black Hole with Schwarzschild radius . This metric assumes that there is only a single Black Hole in the spacetime and that the spacetime in which the Black Hole resides is asymptotically Minkowskian.
Now let’s consider a different scenario. Suppose we have a spacetime which is infinite in space and has an infinite number of Black Holes homogeneously distributed throughout space. If we take a small, spherical region of empty space somewhere far from any one of the Black Holes, this region will be a spherically symmetric vacuum since all the infinite surrounding Black Holes are distributed homogeneously throughout the surrounding space. This region is therefore a spherically symmetric vacuum which must be described by the Schwarzschild metric. Furthermore, just like we are able to model the vacuum around a spherically symmetric distribution of mass by concentrating that mass at a point in the center of the spacetime, we can likewise model our vacuum surrounded by homogeneously distributed Black Holes as being a vacuum with infinite spatial expanse, surrounded by a continuum of Black Holes infinitely far away. We push the infinite number of Black holes out to spatial infinity and by doing so, their combined event horizons appear as a single event horizon surrounding the vacuum.
This scenario must be described by the Schwarzschild metric because we are describing a spherically symmetric vacuum, and the Schwarzschild metric is the only solution to Einstein’s field equation that describes a spherically symmetric vacuum. We know that it cannot be described by the exterior metric because that metric has a Black Hole at its center and is asymptotically Minkowskian (i.e., there are no Black Holes at infinity in the exterior metric). Therefore, this scenario must be described by the interior Schwarzschild metric, which does indeed describe an infinite, spherically symmetric vacuum surrounded by an event horizon.
But given the current understanding of the interior metric, this poses a problem. The interior metric is known as a ’Kantowski-Sachs’ spacetime which has different linear and azimuthal scale factors. This is understood to mean that the spacetime is anisotropic. But the hypothetical scenario described above is isotropic since the Black Holes are distributed homogeneously throughout space and there is no preferred direction when inside the aforementioned vacuum. To reconcile this isotropy problem, we must examine at the Schwarzschild metric in Kruskal-Szekeres coordinates.
The well known Kruskal-Szekeres coordinates, defined in terms of Schwarzschild coordinates are given below. For the exterior metric:
And for the interior metric:
We see that we need separate definitions for the exterior and interior metrics, but we can combine these into a single relationship as follows
Equation
4 is applicable to both the interior and exterior solutions. For the exterior metric,
and for the interior solution,
.
The equation for a 2D hyperboloid surface embedded in three dimensions is given by:
For our purposes, we will be considering the special case where
, which gives the one and two sheeted hyperboloids of revolution. Equation
4 appears to be only for one dimension of space, but if we think of
X as a radius, then it can describe 3 sphrically symmetric dimensions of space.
So comparing to Equation
5, if we set
and
where
R is a radius of a circle in this example, we obtain an equation that matches the form of Equation
5 where :
Equation
6 describes 2D hyperboloid surfaces for a given
r where the interior metric has negative
and the exterior metric has positive
. Let us now visualize a surface of constant
r in both the exterior and interior metrics. For the exterior metric at some
, we get the following hyperbolid of revolution:
On this hyperboloid, the time coordinate t is marked as circles on the sheet and we have one free spatial coordinate on the surface which is the angle of revolution of the surface. This hyperboloid gives us a clear illustration of anisotropy. Event though we are seeing one dimension of space and one dimension of time on the surface, we can see that moving in one direction along the surface (up and down) is different than moving in the perpendicular direction (around the circumference) because one direction is open and infinite and the other is closed.
This is why it is believed that the interior metric, which has the form of a ’Kntowski-Sachs’ spacetime is anisotropic because for the interior metric, the
t coordinate is spacelike and if a 2D spacelike foliation of the interior metric were represented by
Figure 1, than the
t direction of space would be open and infinite, but the perpendicular azimuthal directions would be closed.
However, we need to recall that for the interior metric, the right side of equation
4 is negative, which gives the following two sheeted hyperboloid surface for some constant
:
We will discuss the two-sheeted nature of the surface in a later section, but for now let us focus on one of the sheets in terms of spatial isotropy. To help us interpret the surface, it is useful to look at the 2D Kruskal-Szekers coordinate chart:
Let us focus on region II of the chart. Region II is the 1D representation of the upper surface shown in
Figure 2. What is important to note in this case is that
t is a hyperbolic angle and
is a Killing vector. This means that we can hyperbolically rotate the spacetime to put any point in region II of the spacetime at
without changing the physics. In other words, any point on a given parabola in region II of
Figure 3 can be made the center of the hyperbola by doing a hyperbolic rotation (i.e. there is no intrinsic center for points on the hyperbola, the
point can be any point on the hyperbola). We can say the same with regard to
Figure 2. We can move any point on the hyperbola to the ’apex’ at
by hyperbolically rotating the surface. So the
t coordinate in the metric is akin to a radius for the case where there is no intrinsic spatial center (i.e. one can choose anywhere to be
and then
t increases in all directions away from that point).
So unlike in
Figure 1, where the
t coordinate is timelike, in
Figure 2, representing the interior metric, the
t coordinate is spacelike and has no intrinsic center. But the point on the surface at
sees isotropic space since the hyperboloid looks the same in all directions from that point (note that the same is true in 3 dimensions of space, which cannot be represented here. The only difference in 3D is that the circles shown on the surface in
Figure 2 are spheres). And since any point can be moved to
arbitrarily, this implies that the vacuum is indeed spatially isotropic, in contrast to the exterior metric.
If the interior metric is spatially isotropic as described above, we must now interpret the azimuthal term of the metric which has a temporal scale factor. As can be seen from the metric in equation
1, as
r goes to zero, the
basis vector becomes infinite while the
and
basis vectors go to zero. We can understand this by imagining two circular paths in the interior vacuum passing through the same point as shown in
Figure 4:
What we see in
Figure 4 are two circular paths in the interior metric at some time
r centered on two different points but passing through a common point. The
and
vectors for each path are shown (the particles on each path are travelling counter clockwise). If we were in Minkowski space, the size of these vectors would remain constant over time since the Minkowski metric has no time dependence. But for the interior Schwarzschild metric, the
vectors would grow and the
vectors would shrink over time as a result of the scale factors in front of those terms in the metric.
The way we can understand this is that if we watch a particle in circular motion in the interior metric, we would see the angular frequency of its motion increase inertially over time while still following the same path without any external forces applied to it. This is because as time passes in the interior metric, r decreases and that causes the basis vector to decrease over time such that the circle effectively has a smaller proper circumference over time and therefore it makes a full revolution at a faster rate over time. But the particle does not get closer to the center of the circle over time. Quite the opposite, since the basis vector length goes to infinity as r goes to 0, it gets farther from the center point over time while still travelling a shorter path through spaceitme.
This behavior is supported by the geodesic equation for angular motion [
1] given below (we will examine the case for planar rotation where
).
If we choose
to be
r in this analysis and assume an initial circular motion, we can integrate to get the angular velocity
of the geodesic:
And we see that the angular velocity goes to infinity as
r goes to 0. This can be visualized better by looking at the worldline of a circular orbit in the exterior and interior metrics as shown in
Figure 5:
On the left side of the figure, we see the circular orbit () in the exterior metric with time on the vertical axis and radius on the horizontal axis (a 2D projection of a 3D helix wrapped around the time axis). This a helix with constant radius r. The pitch of the helix is also a constant which means that the angular velocity of the worldline is constant over all time. Since the exterior metric is eternal, this helix can continue as shown for infinite t.
On the right side, we see the same circular orbit (
) in the interior metric. First we note that the signature of the interior metric is flipped relative to the exterior metric and so the vertical time axis is now represented by the
r coordinate and the horizontal space axis is represented by the
t coordinate. Unlike in the exterior case, the interior metric is finite in time, so the worldline can not go beyond
. But we see that the pitch of the helix decreases to 0 as
r goes to zero as though the infinite worldline from the exterior metric has been compressed to fit the finite time of the interior metric. A smaller pitch leads to an increasing angular velocity since it implies more rotations per unit time as
r goes to zero.
Figure 5 therefore shows how the azimuthal scale factor increases the angular velocities of curved geodesics over time without affecting the spatial size of the orbit. This demonstrates how the angular velocity of any size orbit will go to infinity at
.
Therefore, we can interpret the azimuthal scale factor as telling us not that the interior metric is anisotropic, but rather that particles on curved trajectories will experience an angular acceleration over time such that it could take less time to travel on a curved path through space between two points than it would to travel between the same points in a straight line through space.
We will also see in
Section 4.4 that lensed light experiences the same effect where it causes light bent by massive objects to appear more lensed than the mass of the object alone would imply. Therefore, the Dark Matter effects observed from galaxy rotation curves and excess lensing may be attributable to the fact that the vacuum of the Universe is described by the interior Schwazschild metric.
We will provide evidence supporting the cosmological interpretation of the interior metric in
Section 4, but first let us look at what impact the azimuthal scale factor has on the gravitational field of a Black Hole.