2. 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 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].
Figure 1 shows a common depiction of the gravitational well of the Schwarzschild metric (
,
).
We are given the impression here that the geometry inside and outside the event horizon are the same with the main difference being that once an observer crosses the event horizon (), they will continue to fall to the singularity at where they will be ’spaghettified’ as a result of the radius of the 2-sphere collapsing to a point and the t dimension becoming infinitely stretched.
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. As will be shown, space in the interior metric is hyperboloidal, in particular it is a hyperbolic sphere and therefore the space inside the Black Hole is very different than space outside and we seek to fully understand the geometry of the interior metric.
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.
Kruskal-Szekeres Coordinate Chart.
Figure 2.
Kruskal-Szekeres Coordinate Chart.
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. The second thing to notice is that the radius of the sheet is pointed perpendicular to the axis of circular rotation.
So we can see how if in
Figure 3,
r was timelike and
t was spacelike, as is the case in the interior metric, then the spacetime would be anisotropic because in that case, the entire surface is spacelike and the spacetime looks different in different directions. In one direction, the space is closed (moving around a circle on the hyperbolid as
r, which is the time coordinate in the internal metric, decreases), and in the perpendicular direction, the space is open (moving up or down on the hyperboloid).
So if a 2D foliation of the interior metric at some
r was represented by the one-sheeted hyperboloid of revolution (like the exterior metric is), then the common visualization of the gravitational well in
Figure 1 would be correct. However, we need to recall that 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.
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. Recall that
r is now the time coordinate and time is one dimensional, so the radial vector in this case is stuck in one dimension. 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.
Therefore, the t coordinate, which is a hyperbolic angle, is like a ’forward/backward’ coordinate. It represents the straight-line distance from the reference frame to some point. In the exterior metric, the hyperbolic rotation could only happen along one direction (the direction of time), but being spacelike in the interior metric, the hyperbolic rotation can now happen in any direction in three dimensions of 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 to 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. Next, let’s consider motion 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 (
9) 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
:
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 length contraction relative to the
coordinates that makes the slope of the surface at the observer’s location
t more parallel to the
T axis (if the slope is parallel to
T, then
).
Let us consider
Figure 7 which shows a projection of the velocity 4-vector of an orbiting observer on the Kruskal-Szekeres coordinate chart.
We see two components of the 4-vector in this figure, but there is also a 3rd component pointing into the page (the tangential velocity). What we see is that since
is by definition zero for the orbiting observer, as time passes, the worldline follows the line of constant
t that the observer is on. We therefore see in
Figure 7 that the tilt of the
t coordinate line results in a relative velocity of the orbiting observer relative to the
frame in the
X direction (meaning there will be length contraction in the
X direction). This projection is coming from the timelike component of the 4-velocity. We also note that the angle of the velocity vector relative to the
T axis is also equal to
. This does not happen in Special Relativity because the spacelike coordinate lines are parallel to the time axis everywhere in Minkowski spacetime, so there would be no such projection.
So this projection will cause a Lorentz boost of the orbiting frame relative to the
frame as shown in
Figure 8.
On the left, we see the tangent to the surface of a co-moving observer at some location t. When that observer is orbiting, the projection of its 4-velocity onto the X axis causes a Lorentz boost in the coordinates as shown on the right. In this frame, the boost moves the observer outward on the diagram along the hyperbola as the velocity increases. Since is zero, it is the t coordinate lines whose angles are changing that move the points along the hyperbola (so the angle of some t in the comoving frame is smaller than the angle of the same t in the boosted frame). And we can see that as the speed tends toward the speed of light, the angle between the surface at the observer’s location in the boosted frame becomes parallel to and therefore, the angle becomes there (and since the largest possible in the comoving frame is , we see that the boost will increase the angle regardless of the orbit size.
The metric in Kruskal-Szekeres coordinates is given by:
If we solve for
at some
r we get:
Where
and
are functions of the projections of the 4-velocity shown in
Figure 7.
Next we consider the past light cone of a comoving observer at
stretching back to the horizon. Each hyperboloid the cone intersects looks like a celestial sphere to the comoving observer. In
Figure 4, a light cone intersecting the hyperboloid would make a circle on the hyperboloid. But that hyperboloid represents only 2 of the 3 dimensions of space. The third dimension comes from the fact that each of those circles actually represents a 2-sphere since the metric is spherically symmetric. So in the frame of the comoving observer, that observer is at the center of a continuum of isotropic celestial spheres where larger and larger spheres are 2D foliations of space at earlier and earlier times.
We can derive the expression for
t vs.
r along a null geodesic where the geodesic ends at the current time
and
by setting
in Equation (
1) and integrating:
Thus, if we know at which time
r a given sphere is, we can calculate
t for that sphere and use Equations (
7) and (
8) to calculate proper distances on the sphere.
So we are beginning to see that the interior metric is looking a lot like what we observe in cosmology. To the comoving observer, space at a given time is homogeneous and their past light cones show an isotropic spacetime. Next let’s examine what happens when we place a Bleck Hole in this spacetime.
3. A Finite Black Hole Inside an Infinite Black Hole
A black hole embedded in the interior metric is still a spherically symmetric vacuum and is therefore still a valid application of the Schwarzschild spacetime. What we want to know is how does a Black Hole at some fixed time change the spacelike hyperboloidal surface of the interior metric, which itself is a spacelike surface at some fixed time.
First, lets imagine how a surface of constant time t in Minkowski space would be affected by a Black Hole with radius 1.
In
Figure 9, we can think of the vertical coordinate
as the proper time of rest observers. The black line is a line of constant
t, which is the time coordinate of the infinite observer. The curve asymptotes to
as
. We see that at the horizon,
because time dilation is infinite there and so no matter what the value of
t is,
will always be zero. As we move away from the horizon, the ratio
increases until it is 1 at infinity.
This line is a plot of the time dilation of the rest observer in the exterior metric:
Where
in this case. So in Minkowski space without a Black Hole, the
t coordinate line is flat. But when we put the Black Hole in the spacetime, we multiply each point on the line by the time dilation of the rest observer at that point and we see how the spacelike surfaces in Minkowski spacetime are deformed by the Black hole. Furthermore, the slope of the line in
Figure 9 at a point is also the gravitational acceleration at that point given that:
Which is recognizable as the proper acceleration of a rest observer in the exterior Schwarzschild metric.
So to embed the Black Hole in the interior metric, we follow a similar process. Consider
Figure 10.
At the top left, we show the typical visualization of a gravitational well up to the event horizon. To the right, we show the pairs of points representing each circle drawn on the well where the two innermost points represent the event horizon. Note that each pair of points corresponds to a value of t in the interior metric because t is the spacelike coordinate in this metric. Therefore, if we assume a Schwarzschild radius of 1, the two innermost points are at .
We deform the surface on the top right of
Figure 10 one point at a time by first hyperbolically rotating the point to
. We then scale the
value of that point by multiplying it by the time dilation of the rest observer at that point. We then hyperbolically rotate that shifted point back to its initial
t coordinate. Therefore, we can find the new
T and
X coordinates for a given point as follows:
Where
and
T and
X are the original
T and
X coordinates.
Figure 11 shows a plot of the surface with
and
with the undeformed surface shown as a dashed line for reference:
What is most striking about this construction is that in this hyperbolic spacetime, the event horizon is shrunk to a point. So in this spacetime, there is no interior metric inside the Black Hole, the horizon contracts to a point as it is approached and we end at the horizon at .
If we think about orbiting bodies in the exterior metric, a body that has a
that is greater or smaller than
, the geodesic equations will cause the body to tend towards an angle of
and then the orbit becomes stable and
stops changing. So given
Figure 11 and our discussion of
being the angle between the normal of the surface and the vertical, we see that when we have a gravitational well in this spacetime, increasing
to
means that in the frame of the orbiting observer, they will move down the well toward the horizon because at the horizon,
is closest to
. And since this acceleration is infinite as
, we can see that objects stably orbiting a Black Hole in this metric will get pulled to the horizon as
. So if we imagine a galaxy in this metric, it would act as a drain into which everything orbiting it will fall as
.
If we consider systems with small distances and timescales relative to u and t, we see that the vacuum spacetime of that region is approximately flat because that is the region close to the apex of the hyperboloid at (the r and t coordinates there are approximately perpendicular and light travels on 45 degree lines). Therefore, when we add a gravitational well of say, a star, in that region, it will look like a little divot in the surface and as long as we are not near or , it is as though the well is constructed on top of Minkowski space and therefore behaves like the exterior metric. Thus, we expect to see the acceleration of orbiting observers described by this metric to be observable at relatively large scales whereas the effects become negligible at relatively small scales (when we are sufficiently far from and ).
Thus, we have shown that in the frame of the comoving observer, the interior metric looks isotropic and that it also looks homogeneous at a given past time. Then we showed that a Black Hole can be embedded into this spacetime such that it has no interior. Therefore, it is time to examine this metric in the context of cosmology because we have shown all the properties of the Cosmological Principle in this spacetime and therefore what we potentially have here is a model for the Cosmological vacuum.
We have inserted a single Black Hole into the spacetime, but if we homogeneously and isotropically distribute Black Holes throughout the infinite Universe, we would also have a spherically symmetric vacuum. And since the horizons of these Black Holes reach back to (the surface of the shell), then cosmologically speaking, we can say that the interior Schwarzschild metric is the correct description for the spacetime of the cosmic voids of our Universe. If there are an infinite number of Black Holes in the Universe and their horizons are at , then we see that from any vantage point in the vacuum, there would be a horizon in every single spacelike direction (not that we could see a Black Hole in every direction, just that at least one exists in every direction at some arbitrary distance t from us at all times) and those horizons together make up the shell that surrounds the Universe at .