3. Analysis of the Geometry of the Interior 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 a point at the center of the spacetime.
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 [
1].
Since
r is spacelike in the exterior metric, at constant
r, space is a 2-dimensional spherical surface. But in the interior metric, a surface of constant
r is a 3-dimensional spacelike volume. This means that
r in the interior metric is related to cosmological time. So in terms of the voids, this means the spatial distance from the center of the void to its surface is measured by the
t coordinate in the metric, not
r. As will be shown in
Section 4, the
r coordinate is related to the scaling of the void over time, indicating that the size of a void is also related to its age, where larger voids would, in many cases, be older than smaller ones. So regardless of their respective spatial sizes, the
r coordinate of all voids at a given cosmological time is the same.
So we need to examine the exterior and interior geometries more closely to understand how exactly they are different, particularly in regards to the meaning of the azimuthal term in each case. The Kruskal-Szekeres coordinates are very useful for this task. As we will see, the Kruskal-Szekeres coordinate chart allows us to see how the
t and
r coordinates are curved relative to Minkowski space. But first, we define the Kruskal-Szekeres coordinates in terms of the Schwarzschild coordinates. For the exterior metric:
And for the interior metric:
With these definitions, we can plot the Kruskal-Szekeres coordinate chart [
2]:
Figure 2 is perhaps one of the most beautiful charts in all of physics. It essentially overlays the geometries of all three spherically symmetric spacetimes described by the Schwarzschild metric overlaid on one another so that the geometries can be easily compared. We have the exterior metric in regions I and III, the interior metric in regions II and IV, and the Minkowski metric over the entire chart represented by the T-X coordinate grid (remove the
r and
t coordinates from the chart and you are left with Minkowski spacetime). Visualizing the differences in these geometries relative to each other will be crucial for understanding the interior spacetime
In this paper, we will focus primarily on regions I and II of this chart, representing the exterior and interior metrics respectively. Since the Kruskal-Szekeres coordinates are defined in such a way that null geodesics are 45 degree lines everywhere on the chart and the T and X coordinates are straight and mutually perpendicular everywhere on the chart, we can think of the T-X grid as Minkowski space with the curved r and t coordinates overlaid on the grid. Thus, this chart clearly shows how the Schwarzschild space and time coordinates r and t are curved relative to the Minkowski coordinates T and X. We see that the r coordinate lines are hyperbolas, which captures that fact that an observer at rest in the exterior metric experiences a constant acceleration, and the t coordinate is a hyperbolic angle. That t is a hyperbolic angle will become an important fact when we look at the geometry of the interior metric.
We see from equations
2 and
3 that we need separate Kruskal-Szekeres coordinate 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. The location is at the throat of the hyperboloid. The first thing to note here is that the t coordinate can only be hyperbolically rotated in one direction: up or down. This is because the t coordinate is the coordinate of time and time only has one dimension so there can only be a hyperbolic rotation along the single time dimension. We also see in this figure that the circles, which all have the same r value, seem to grow as t increases. It is as though each surface of constant r gets bigger in the time dimension as t increases, which reflects the fact that an observer at rest on the surface feels a constant acceleration from this growth of the surface in the time dimension.
For the interior metric, the right side of equation
4 is negative, which gives the following hyperboloid surface for some constant
:
The first thing we notice is that this is a two-sheeted hyperboloid, which is known as a hyperbolic sphere, as opposed to the one-sheeted hyperboloid of the exterior metric. So right away, we can see that the interior and exterior geometries are different. We should also note that for Minkowski space, the surface equivalent to
Figure 3 and
Figure 4 would be a cylinder.
If we look at region II of
Figure 2 in the context of
Figure 4, we see that in contrast to the exterior metric where the radius is perpendicular to the axis of circular rotation, in the interior metric, the radius is parallel to this axis. Furthermore, we see that the
t coordinate, which is a hyperbolic angle, can be rotated in 3 different dimensions now since the
t coordinate is spacelike (we see two of the three dimensions in
Figure 4). Since
t is a hyperbolic rotation and
is a Killing vector of the spacetime, we can hyperbolically rotate the space to move any point on the surface to
which is at the apex of the hyperboloid. So just like we can set any arbitrary time as
in the exterior metric, we can set any arbitrary location as
in the interior metric. In particular, for a given comoving frame we are examining, we can say that that comoving frame is always at
, and when the frame moves in a straight line (along a hyperbola) in a particular direction, that is modeled as the hyperboloid being hyperbolically rotated in that direction such that the reference frame remains at
as it moves.
It is important to note here that real Black Holes, which are described by the exterior metric, are not eternal (they only exist for some finite t) and likewise real voids, which are described by the interior metric, have finite sizes (they only occupy some finite distance t in space).
This brings us to the azimuthal term of the interior metric. Consider
Figure 5 which depicts the parallel transport of a normal vector of a spherical surface around a line of latitude of the sphere.
On the left side of the Figure, we see the normal vector being parallel transported, and on the right, we see how that vector precesses as it is transported. So for the exterior metric at some r, the precession of the normal vector as it is transported around the loop gives us the and values of the path that are used in the metric. The important thing to note here is that will increase or decrease as the path moves toward or away from the pole of the sphere.
In the interior metric, space is hyperboloidal, but we can use the same technique transporting a normal vector around one of the sheets (the top sheet in this analysis) to help us understand the angular term of the interior metric.
Figure 6 shows how
and
are defined for the interior metric.
As was the case for the sphere, is the angle of revolution of the transported normal around the central axis while is the angle of the normal relative to vertical. So at , and increases as we move away from . One thing making the hyperbolic geometry different than the spherical geometry is that as , in the interior metric. This means that while on the sphere of the exterior metric, , in the (unaltered)) interior metric, .
Since the surface in
Figure 4 is at constant
r, which is a time, we see that
and in particular
acts like a spatial radius, giving the spacelike circles on the surface different circumferences even though they are all at the same radius.
Let us us calculate the proper circumference of one of these circles. The circle has
and noting that
in equation
1, the proper circumference will be given by:
We can relate
of a given circle to
t in this context by noting that the slope of the surface tangent is given by
. The angle between the tangent vector and vertical will be equal to the angle between the normal and the vertical and is given by:
And so we can calculate the value of
from
t. We can also look at this another way. Consider
Figure 7 where we are looking down at one of the spacelike hyperbolic surfaces at some
from the hyperbola at
.
First note that all the circles in this figure have the same value of r, but represents the center of rotation and circles of larger t are points farther away from and therefore must have larger proper circumferences as t increases.
Circles in this figure are analogous to lines of latitude on a spherical surface around an arbitrary pole at . So the radial vector is pointing straight into the page at (so at ) and has some angle when pointing to any circle. Thus, the circumferences of the circles get larger as t gets bigger because increases as we move to larger t and the portion of the radius normal to the circle is , which would be the effective radius of the circle.
We can also see this on the spacetime diagram where
is represented not by a point, but by a hyperbola. So on this diagram, radial lines are lines of constant
t (because
along these lines).
Figure 8 shows the radial line for a comoving observer (center) and an observer revolving around
on the Kruskal-Szekeres coordinate chart.
At
, the radial vector is parallel to the axis of rotation (this is analogous to the radial vector pointing straight up in
Figure 5). But at
, the radial vector is angled relative to the rotation axis and that angle is given by
(analogous to
r pointing to one of the lines of latitude on the sphere in
Figure 5).
Now let us consider how we measure distances on a spherical surface at some
. As has been discussed, each circle on the hyperboloid is in fact a spacelike 2-sphere such that at a given surface of
r, each circle of constant
t represents a sphere at some distance
t from the center at
. Thus the full 3D space at a given
r is modeled as a set of concentric spheres that get larger as the magnitude of
t increases. All the points on such a sphere will have the same
X and
in equation
4. The
t coordinate on these spheres are lines of latitude around some chosen axis.
Figure 9 shows one such sphere where the equator of the sphere would be represented on the hyperboloid of
Figure 4 as a circle of constant
t.
We want to know how to calculate the circumference of the line of latitude shown on the sphere which is at some angle from the vertical polar axis. The radius of the sphere in the Kruskal-Szekeres X-coordinate is . Therefore, the radius of the circle of latitude shown will be given by .
Note that the sphere is in the 4th dimension with respect to the hyperboloid surface in
Figure 4 (only the equator is visible in that figure, but the rest of the sphere would extend into the 4th dimension since that figure is showing 2 dimensions of space and 1 dimension of time). As has been mentioned, all points on the sphere are at a constant
X and
in equation
4 and therefore, according to equation
4 all points also have the same value of
T. Therefore, since we cannot draw a 4D image of the spacetime, we can instead project the lines of latitude of the sphere onto the plane of the equator, which is a plane of constant
T as shown in
Figure 10.
So we know the value of
t at the equator (it is chosen) and now we want to know what the value of
t is for the line of latitude in question. The value of
X at the equator is
and at the line of latitude it is
. The value of
T is the same in both cases, and if we divide the definitions of
X and
T in equation
3 and solve for
T to get:
Since
T is the same for the equator and the line of latitude:
Where
is the value of
t at the equator and
t is the value of
t at the circle of latitude. Rearranging, we get:
And finally, we can solve for the
of the circle of latitude using the relationship from equation
8, giving:
Therefore, we have a more general equation for finding
on a sphere for a circle of latitude given the size of the sphere (
) and the angle
which is the angle of the circle of latitude as measured from the spatial center of the sphere. And since we know
r, we can use equation
7 to then calculate the circumference of the circle of latitude.
Let us next consider what a comoving observer at some
sees in their past light cone. We can derive the expression for
t vs.
r along a null geodesic where the geodesic ends at the comoving observer’s time
and
by setting
in Equation (
1) and integrating:
The observer will see concentric spheres around them with the size
of each sphere on the light cone given by equation
13 in terms of
r of the sphere and
of the observer. Given the spherical symmetry, we can conclude that in the frame of the comoving observer, each sphere is homogeneous and isotropic, and therefore the observer sees a spacetime which satisfies the Cosmological Principle.
There is one more way to look at this, and that is from the frame of the orbiting observer. Imagine an observer that travels in a straight line for some time and then transitions to a circular path of some arbitrary size. In this situation, we will keep the observer at
and move the spacetime relative to the observer.
Figure 11 depicts such a situation.
On the left side, we see the situation of the observer moving in a straight line. The spacetime is hyperbolically rotated in the direction of travel while the observer is kept at
. When the observer transitions to circular motion, we have the situation on the right side of
Figure 11. Since we are keeping the observer at
, then during the circular orbit the spacetime is spherically rotated about the axis at the center of rotation where the axis is normal to the surface at the center of rotation at some
in this picture. Because the axis is normal to the surface, the angle between the rotation axis and vertical axis is
and we can most clearly see how
becomes the radius of the orbit. And if we hyperbolically rotate the spacetime on the right side of Figure to put the center of rotation at
, then we get the same picture we examined previously.
Next, let’s consider acceleration around one of these circles. In this case,
along the path. The geodesic equations for
and
are given below [
3] where we use
as the affine parameter.
Since we are moving on the circle, the initial condition is that
. We see from equation
14 that even though we start with a constant
, there will still be a change in
over time since
is not zero.
So what is of interest here is that
is changing over time even though the initial
was constant. This suggests the particle is changing its distance from the
point along the hyperbola. However,
still remains constant because the angular geodesic equations are not functions of
t, nor is the geodesic equation of
t a function of
or
(and we are forcing
for this situation):
In this case, in the observer’s frame, the circles must be decreasing or increasing in size (depending on the sign of ) over time. The value of t remains constant at all times, so this suggests that the cause of the increase in must be due to a Lorentz boost.
If we first consider only the comoving observers on the Kruskal-Szekeres coordinate chart, these observers move along lines of constant
t. This means their time axes are tilted relative to each other, indicating they are moving away from each other over time with some relative velocity which is a function of
between the observers we are comparing. Since all comoving observers are moving away from each other, the space is expanding in this metric. This will be investigated more thoroughly in
Section 4, but it turns out the expansion is not constant over time. This is because the hyperbolas of constant
r are not equally spaced along the
T axis (
is a function of
r, not constant). This expansion will help us understand why orbiting observers accelerate over time.
Consider
Figure 11 which shows the frame of a comoving observer at some
relative to a
observer on the Kruskal-Szekeres coordinate chart.
It is notable here that the angle between the
T and
axes in
Figure 11 is also
. As mentioned, the comoving observer whose vector is shown in the diagram is moving away from the observer at
because their time axes are tilted relative to each other. So the observer at
has a velocity in
X relative to the
observer.
Now, if the observer starts moving on the circle of constant
t, it will have a velocity component tangent to the circle (
) from the circular motion, but it will also still have a velocity normal to the circle (
) due to the tilt of the time axis. The effect that the normal velocity has on the tangential velocity as the observer moves around the circle is shown in
Figure 12.
In this diagram, we see the orbiting observer’s velocity components at some time
r and some later time
. If this was in Minkowski spacetime,
would be zero, and we would have constant circular motion with a centripetal acceleration caused by
. But here, we have the normal velocity
, and since that velocity is always normal to the circle,
will always point in the tangential direction. Therefore, the
will add to the
velocity, causing an acceleration in the tangential direction (a kind of Coriolis acceleration). This acceleration will increase the Lorentz boost of the frame relative to the comoving observer at
t, increasing the value of
for the orbiting observer over time, as shown in
Figure 13, where the frame of the orbiting observer is given by the
and
axes.
Now that we have established the geometric features of the interior metric, let’s compare the metric to observational data to show that modeling the voids using the interior metric allows us to explain the accelerated expansion of the Universe without the need for a non-zero Cosmological constant.