The Helland universe (part 2 of 4)
This is the second of a 4-part series that analyzes the Helland universe.
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The Helland universe in spherical coordinates.[/size]
These three coordinate systems use spherical coordinates to describe spatial dimensions of the Helland universe. They differ only in their radial coordinates: r, q, or ρ.
Radial coordinate r
The Helland metric form,
as stated by Mike Helland on 26 October, uses a radial coordinate r that is restricted to the range 0 ≤ r < 1.
ds2 = − (1 − r)−2 c2 dt2 + dr2 + r2 [ dθ2 + sin2 θ dφ2 ]
For any fixed value t
0 of the time coordinate t, the set of all spacetime events with coordinates of the form (t
0, r, θ, φ) is called a
spatial slice of the spacetime manifold.
Using spherical coordinates for spatial dimensions emphasizes the spherical symmetry of spatial slices around the central event E
0. In this coordinate system, E
0 has coordinates (t
0, 0, 0, 0).
If t
0 = 0, that central event happens to be the origin of this particular coordinate system.
Whether there is anything special about that central event is an important question. That question can be answered by calculating the
Ricci scalar field and comparing its value at the origin to its value at other events within the same spatial slice, but it is easier to answer the question by transforming the metric form into a Cartesian coordinate system as will be done in a later section.
In the metric form above, the coefficient of dt
2 is
gtt = − (1 − r)−2 c2
The presence of that radial coordinate r within g
tt suggests the Helland universe is neither homogeneous nor isotropic, and that events at the origin of a spatial slice are indeed special. We need to be cautious when drawing such conclusions, however, because is possible for a coordinate system to disguise the homogeneity and isotropy of a manifold. The
Rindler coordinate system is a standard example of this phenomenon.
Another important question is whether the Helland universe is static. Apart from a
few very special exceptions, the FLRW models of mainstream cosmology are not static, because they describe universes that are always expanding or contracting.
The time coordinate t does not appear within the Helland metric form, which implies the metric tensor field is the same for all spatial slices, which means the Helland universe is static from the point of view provided by this coordinate system.
It is possible to devise a coordinate system in which the Helland universe appears to be nonstatic. Consider, for example, an observer in motion whose r coordinate increases with time. If we were to transform into a coordinate system in which that observer is at rest with respect to the spatial coordinates, then the Helland universe would not be static from the point of view provided by that coordinate system. As will be shown by the seventh coordinate system considered in this essay, that observer (considering himself to be at rest) would see the coordinates of the universe's center changing over time.
It is conventional, however, to say a universe is static when its most natural coordinate systems provide a description in which all spatial slices have the same metric tensor field. In the first six coordinate systems described within this essay, the Helland universe is static. The fact that those coordinate systems agree upon this point makes it reasonable to say the Helland universe is static.
Radial coordinate q
The origin of a coordinate system is essentially arbitrary. A coordinate transformation that simply moves the origin to some other place is called a
translation.
With Cartesian coordinate systems, translations are easy because they are performed by adding a constant (possibly zero) to each coordinate.
With spherical coordinate systems, translations can be messy because (in general) the angular coordinates must be adjusted in nonlinear fashion.
As a sort of warmup exercise, consider the coordinate transformation that leaves the t, θ, and φ coordinates unchanged but replaces the radial coordinate r by a new coordinate q = r − ½, where −½ ≤ q < ½. In this new coordinate system, the central event E
0 has coordinates (0, −½, 0, 0). A different event E
1 has coordinates (0, 0, 0, 0).
Whether we regard E
0 or E
1 as the origin of this new coordinate system is a matter of taste, but it is important to understand that the angular coordinates θ and φ are still defined with respect to the spatial position of E
0.
Whether we regard q as a radial coordinate is another matter of taste. I will refer to q as a radial coordinate, but some may insist that a coordinate that can have negative values should not be regarded as a radial coordinate. Regardless, it is important to understand that using q instead of r is a legitimate coordinate transformation.
Finally, it is reasonable to question whether the q-coordinate system should be regarded as a spherical coordinate system at all. The fact that its angular coordinates are defined with respect to a point other than the origin argues against thinking of it as a spherical coordinate system. Regardless, it is important to understand that the q-coordinate system is a perfectly legitimate coordinate system.
When transformed to use q instead of r, the Helland metric form becomes
ds2 = − (½ − q)−2 c2 dt2 + dq2 + (q + ½)2 [ dθ2 + sin2 θ dφ2 ]
By substituting r − ½ for q throughout that metric form, it is easy to prove that this transformed metric form is equivalent to the Helland metric as originally stated by
Mike Helland using the r-coordinate system.
Note, however, that the algebraic simplicity of that proof depends upon the fact that dq = dr. If the relationship between q and r were non-linear, we would have to use calculus to derive the relationship between dq and dr.
Radial coordinate ρ
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Notation:
In this section, the Greek letter ρ (rho) is used as a radial coordinate. That radial coordinate has nothing to do with the mass-energy density corresponding to
the stress-energy tensor's Ttt component, for which ρ is a common notation. To reduce confusion, I will write ρ
m for the mass-energy density when I discuss it in a later section.[/size]
In the original r-coordinate system, the fact that r is restricted to r < 1 might cause some people to wonder whether the Helland universe is bounded by some sort of wall. Would an observer moving toward increasing values of r eventually run into that wall? Or fall off the edge of the Helland universe?
The answer to both of those questions is that it is impossible for an observer ever to get to r = 1, because there are no events of the Helland universe for which the r-coordinate is 1.
That is not a terribly satisfying answer. Some people might prefer a radial coordinate that ranges over all non-negative real numbers.
We can accommodate their aesthetic concern by transforming from the r-coordinate system to a system that leaves the t, θ, and φ coordinates unchanged but replaces the radial coordinate r by a new radial coordinate ρ = r/(1−r) = 1/(1−r) − 1.
From that relationship between ρ and r, it is easy to see that the possible values of ρ should include all non-negative reals.
When transformed to use ρ instead of r, the Helland metric form becomes
ds2 = − (ρ + 1)2 c2 dt2 + (ρ + 1)−4 dρ2 + (ρ / (ρ + 1))2 [ dθ2 + sin2 θ dφ2 ]
To prove this metric form is equivalent to the original Helland metric form, one must prove that
dr = (ρ + 1)−2 dρ
That's just a matter of calculating dρ/dr and applying some high school algebra.
Having proved that the three coordinate systems defined above yield equivalent metric forms, we know those three metric forms all describe exactly the same metric tensor field.
We can therefore use any of the three coordinate systems to reason about the Helland universe.
We have to be careful, however, because all three of those coordinate systems have a coordinate singularity at the central event E
0 and at all other events whose spatial coordinates are the same as those of E
0.
Coordinate singularities
Suppose some intrepid adventurer tells you his expedition plans to ski southward from McMurdo Station until they reach the South Pole. From there they will head north until they reach the Antarctic coast, where you are expected to pick them up.
Does that plan tell you where they expect you to pick them up? No, it does not.
At most places on earth, what we mean by "north" is well-defined. At the South Pole, however, "north" is not well-defined.
That is an example of a coordinate singularity.
Informally, a coordinate singularity is a place where something goes haywire, typically because some coordinate or direction or derivative is not well-defined.
Spherical coordinate systems have two distinct kinds of coordinate singularity. One kind of coordinate singularity occurs with the angular coordinates because an angle of 0° is the same as an angle of 360°. Those coordinate singularities are typically handled by restricting the range of an angular coordinate, as by saying 0 ≤ θ < 2π.
Even with that convention, the coordinate singularity at θ=0 remains problematic because the mapping from points to their θ coordinates is discontinuous at θ=0, which causes derivatives involving θ to become undefined.
That is why the mathematical definition of a Riemannian or pseudo-Riemannian manifold insists that coordinate charts be defined on open subsets of the manifold, and that the mapping from points in that open set to their coordinates be continuous and sufficiently differentiable.
That is also why the surface of the earth cannot be covered by a single chart. You can't flatten the earth's surface (which is homeomorphic to a 2-sphere) onto 2-dimensional Euclidean space without puncturing or tearing the 2-sphere.
The surface of the earth can be covered by two charts that overlap at their boundaries. That is the mathematical basis for the idea that "Well that's no problem, you can just rotate the spherical coordinates a little bit if you're trying to do calculations at that boundary."
As an example of that workaround, consider the g
φφ component of the Helland metric form in the r-coordinate system:
gφφ = r2 sin2 θ dφ2
That is the g
φφ component of the covariant metric tensor. When we calculate the Ricci scalar in the next subsection, we will need to calculate the g
φφ component of the contravariant metric tensor, which is related to g
φφ by
gφφ = 1 / gφφ
When θ is zero, sin θ is zero as well, so g
φφ = 0 and our calculation of g
φφ has to divide by zero.
We can avoid that by taking care to use nonzero values of θ whenever we calculate the Ricci scalar. Because the Helland universe is spherically symmetric, the Ricci scalar will be the same for θ = π/2 as for θ = 0, but you can see how this coordinate singularity makes the Ricci scalar slightly harder to calculate, and we'd have a more serious problem if we were calculating the Ricci scalar for a spacetime manifold that isn't spherically symmetric.
Spherical coordinates have another coordinate singularity involving the radial coordinate, because the angular coordinates are not well-defined at r=0. That coordinate singularity is typically handled by a convention that says the angular coordinates are zero whenever r=0.
Even with that convention, the coordinate singularity at r=0 remains problematic because the mapping from points to their angular coordinates is discontinuous at r=0, which causes derivatives to be undefined at r=0.
And that coordinate singularity definitely impedes analysis of the Helland universe at r=0, which is a serious problem because one of the most important questions we want to answer is whether points whose r-coordinate is zero actually represent a special center of the Helland universe's spatial slices.
One way we might try to answer that question is to look at the behavior of the Ricci curvature tensor.
Mike Helland has calculated the components of that tensor for his r-coordinate system, from which we see that the R
tt component of that tensor blows up (becomes infinite) at r=0. That suggests a point at r=0 occupies a special place in the Helland universe, and likely represents the center of the Helland universe.
But wait a minute! We ought to consider the possibility that the Ricci tensor blows up at r=0 because of the coordinate singularity at r=0, and that the components of that tensor at such points might be well-behaved if we were using some other coordinate system.
In short, coordinate singularities make it difficult to draw reliable conclusions at those singularities or in their vicinity.
To draw reliable conclusions, it is often best to transform into a coordinate system that doesn't have coordinate singularities in the region of interest.
Ricci scalar
The Ricci scalar R is the trace of the Ricci curvature tensor, and can be computed from the diagonal components of the Ricci tensor using the following equation, in which summation is implied by the Einstein summation convention.
R = gii Rii
The index i ranges over the four coordinates t, r, 0, and φ, the g
ii are components of the contravariant metric tensor, and the R
ii are components of the covariant Ricci tensor.
As was explained in the previous section, a coordinate singularity leads to division by zero in that equation unless we take care to work around the problem.
Unlike the coordinate-dependent components of the metric tensor and Ricci tensor, the Ricci scalar is an invariant that does not depend on the coordinate system. If we calculate the Ricci scalar correctly, avoiding coordinate singularities, it may tell us whether the Helland universe's curvature varies from point to point.
The following graph, which relies upon
Mike Helland's calculation of the Ricci tensor, shows that the magnitude of the Ricci scalar does indeed vary as a function of the radial coordinate r.
The Ricci scalar is negative throughout the Helland universe, so that graph shows the logarithm of its absolute value. On the horizontal axis, lg r = -30 is less than one millimeter, while lg r = -1 is 1.38 billion light years.
As can be seen from the log-log graph, the Ricci scalar converges to negative infinity as r approaches zero.
That tells us the Helland universe is not homogeneous and is not isotropic.
That graph also tells us the Helland universe is geocentric in the sense of having a spatial center at r=0 at which the curvature is far greater than at any other point of space, and the spacetime curvature is spherically symmetric around that center.
Coordinate speed of light
We can use a metric form to calculate the coordinate speed of light at various points of a spacetime manifold.
The coordinate speed of light seldom tells you anything interesting about the physics, because it has more to do with the coordinate system than with physical reality, but the coordinate speed of light can tell you something about the coordinate system.
Consider a photon moving directly away from the r=0 origin of the r-coordinate system. Its angular coordinates don't change, so dθ = dφ = 0. Photons travel along null geodesics, so
ds2 = 0 = − (1 − r)−2 c2 dt2 + dr2(1 − r)−2 c2 dt2 = dr2dr/dt = (1 − r)−1 c
dr/dt = c/(1 − r)
That tells us the coordinate speed of light depends upon the r-coordinate of the photon. The coordinate speed of light is c at r=0 and increases as the photon moves further away from r=0.
Points with r=0 are the only points of the Helland universe at which the coordinate speed of light is c. Does that mean points with r=0 are special?
Not necessarily. The fact that points with r=0 are the only points at which the coordinate speed of light is c might be a fairly meaningless artifact of the r-coordinate system.
Let's calculate the coordinate speed of light in the ρ-coordinate system:
ds2 = 0 = − (ρ + 1)2 c2 dt2 + (ρ + 1)−4 dρ2(ρ + 1)2 c2 dt2 = (ρ + 1)−4 dρ2dρ/dt = (ρ + 1) c / (ρ + 1)−2dρ/dt = c (ρ + 1)3
Points with ρ=0 are the only points of the Helland universe at which the ρ-coordinate speed of light is c. The ρ-coordinate speed of light increases as the photon moves further away from ρ=0.
At event E
0, the coordinate speed of light is c in both of those coordinate systems.
Let's calculate the coordinate speed of light at E
1, whose q-coordinates are (0, 0, 0, 0).
In the r-coordinate system, the coordinates of E
1 are (0, ½, 0, 0) so the r-coordinate speed of light at E
1 is c/(1 − ½) = 2c.
In the ρ-coordinate system, the coordinates of E
1 are (0, 1, 0, 0) so the ρ-coordinate speed of light at E
1 is c (1 + 1)
3 = 8c.
E
1 is a point of the spacetime manifold, and that point doesn't change just because we decide to express its coordinates using a different coordinate system. In physical reality, the actual speed of light at E
1 has to be exactly the same as the actual speed of light at E
1.
But the coordinate speed of light at E
1 depends on your choice of coordinate system.
Using a coordinate speed of light to draw conclusions about physical reality is like using a Mercator map to compare the areas of Greenland and Africa.
It might be a good idea to consult more than one map.
A man with only one watch knows what time it is.
A man with two watches is never quite sure.
The man with two watches is less certain because he knows more than the man with only one watch.