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Can the equation of spacetime be local for a balloon model?
Let us think of the Schwarzschild solution. The solution extends through the entire asymptotically Minkowski space. The central mass M affects locations very far away.
For a spherical rubber balloon, the equation governing its stretching is local, if we assume that the pressure inside is uniform.
Friedmann equations in general relativity look local, but that is only because we assume a uniform mass distribution. Any retardation effects are masked.
A rubber string and a weight
rubber string
●----------------------------●
point point
Let us draw points uniformly around a sphere, and connect them with tense rubber strings which run on the surface of the sphere. The rubber strings simulate the gravity between the mass points. If the balloon is static, or inflates or deflates at a constant rate, this model looks like an ordinary balloon: the tension in the strings is uniform along the string.
A rubber string and a weight which the string slows down
Let us consider the simplest possible model of a tense rubber string plus weight:
force
F <------
==| ~~~~~~~~~~~~~~ ● ---> v
wall rubber string M weight
We are interested in what kind of longitudinal waves form in the string when the weight moves to the right while the tension in the string pulls the weight to the left.
Free waves in the string are sine waves. Since the speed of the waves is finite, there is "retardation".
As the weight slows down, it creates new waves. The weight perturbs the string. Calculating the precise form of the wave probably requires a computer. But we are only interested in very crude estimates.
Do binary pulsars prove that there are no longitudinal gravitational waves? Are longitudinal waves confined between masses?
Binary pulsars have confirmed that transverse waves and linearized Einstein field equations explain the energy loss of a binary pulsar up to a precision of 0.1%.
In an earlier blog post we suggested that longitudinal waves must be "absorbed into" matter quickly, because they cannot propagate in empty space. This hypothesis would explain why binary pulsars match the transverse wave model so well.
Another hypothesis: longitudinal wave effects can only exist in the field between two masses M₁ and M₂ and can never escape to empty space.
Longitudinal electromagnetic waves exist in plasma, but they do not exist in empty space. Could this be analogous to our model of retarded gravity? Langmuir waves exist in a plasma which is, on the average, neutral. Since gravity charges always are positive and gravity always pulls, Langmuir waves cannot exist in a gravitating system.
A model with solid rubber inside
Let us have two masses M₁ and M₂ on the surface of the balloon. Visualizing a rubber string between the masses, and running on the surface of the balloon, is somewhat hard. Let us imagine that the rubber string runs inside the balloon.
The simplest case is when M₁ and M₂ are on the opposite sides of the balloon. A rubber string runs through the center of the balloon and connects them.
The balloon expands. The rubber string is not immediately aware of the expansion slowing down. This will cause oscillation in the expansion rate.
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Let us have a solid rubber ball. The rubber will resist the expansion in most cases. But if there is a shock wave moving from the center toward the surface, the expansion of the rubber ball may actually accelerate at a certain time. "Dark energy" in this case is the energy of the shock wave.
This model predicts that the expansion rate of the universe will oscillate, while it, on the average, is quite similar to an FLRW model.
But we should find a mathematical formula, so that we could compare it to the observed dark energy.
The strength of dark energy seems to be weakening right now
The DESI project measures the 3-dimensional mass density variations of the universe right now, and compares it to the baryon acoustic oscillations after the Big Bang. The results of DESI, when combined to other observations, suggest that dark energy is weakening right now. Wikipedia says that dark energy density right now might be 10% less than 4.5 billion years ago.
This is consistent with our own rubber ball model: on the average, the expansion should be like an FLRW model, but there should be "bounces" from the retardation of gravity.
In the link we have the definition for the CPL parametrization of the dark energy equation of state, w(a), where a is the universe scale factor. The current value of a is set to 1.
Abdul-Karim et al. (2025) write that the energy density of dark energy may have increased in the past. This is called a "phantom crossing". In our rubber ball model, a phantom crossing is expected: at some points the bouncing slows down the expansion, at other points speeds up the expansion.
The Hubble tension
Let us measure the baryon sound horizon size in the cosmic microwave background, and match it to the measured density fluctuations in the current universe. Assuming, for example, the standard ΛCDM model, we end up with a Hubble "constant" current value of
67 km/s / Mpc.
But a direct measurement, based on Cepheids and type 1a supernovae yields a value
73 km/s / Mpc.
The values differ too much to be just a statistical fluctuation.
Marco Raveri (2023) tries to use dark energy to make these values compatible. Let us check what he suggests. His conclusion is that dark energy modifications at "late" times, 0.01 < z < 3 cannot solve the Hubble tension.
Early dark energy (EDE)
Xuejian Shen et al. (2024) write about an early dark energy (EDE) model, where an unknown field boosts the expansion of the universe just before the recombination (last scattering) which happens when the universe is 380,000 years old in a standard ΛCDM model.
Shen et al. say that this model can solve the Hubble tension. Is it so?
Let us start from the observed uneven matter distribution in the recent universe, and match it to the the uneven matter distribution in the cosmic microwave background (CMB). The baryon acoustic oscillations (BAO) make bumps into the uneven distribution. Let us match the bumps in recent matter and in the CMB.
Let us calculate time backward from the present time, and model matter distribution at earlier times. We use a standard ΛCMB model. When the universe has shrunk to one 1,100th of its size, the CMB has a temperature of 3,000 K, and the last scattering occurs.
The Hubble tension is that the BAO bumps in this calculation have a larger angular scale than in the measured and mapped CMB in the sky. That is, the "features" in the actual CMB map are smaller than our calculation backward in time predicts.
The early dark energy (EDE) hypothesis talks about what happened before the last scattering. The hypothesis does not help in any way in solving the Hubble tension. We have to check the literature. Can the EDE hypothesis be so much wrong?
Karsten Jedamzik et al. (2020) write that EDE cannot resolve the Hubble tension.
Above, θ* is the angular size of the sound horizon, that is, the angular size of "features" in the CMB. We use coordinates comoving with matter. Then r* is the spatial size of the sound horizon (in those coordinates), and D(z*) is the spatial distance to the last scattering.
Jedamzik et al. say that only the quantity
Ωm h²
affects the spatial distance to the last scattering, in a flat ΛCDM model. There, Ωm is the matter fraction of the critical density, and h is the value of the Hubble constant now.
The authors state that the Dark Energy Survey and the Kilo-Degree Survey have set strict limits on Ωm h², so that any attempt to solve the Hubble tension through manipulating Ωm h² will fail.
Let us check what they say about manipulating r*. Suppose that we calculate the development of a ΛCDM model backward in time. The matter density variations of galaxy clusters eventually turn into variations of the CMB as the temperature rises.
Solving the Hubble tension with a very slow expansion during the first billion years of the universe: also the James Webb paradox of too mature galaxies is solved
The James Webb telescope has observed galaxies which in a standard ΛCDM model are only 500 million years old, but look much more mature, as if they were 1.5 billion years old.
Let us assume that the expansion during the first billion years of the universe was much slower than the ΛCDM says. We add an "extra" 1 billion years to the age of the universe, to the early phases of the universe. Adding that extra means that the universe expands much slower than in the ΛCDM model, during the first 1 billion years or so.
Then galaxies have much more time to mature. This solves the James Webb paradox.
During that slow expansion during the first 1 billion years, photons from the last scattering had time to move a "longer" path than in the ΛCDM model. Let us explain what "longer" here means. If we model the expanding universe with coordinates comoving with matter, then the ruler of the spatial metric (say, a ruler 1 meter long) shrinks as time progresses. The "length" of the path of the photons is measured in these comoving coordinates.
Since the photons moved a longer path before coming to our eyes, the features in CMB will have smaller angular diameters in our eyes. This resolves the Hubble tension.
Let us make a quantitative calculation. We assume a matter-dominated universe with a zero pressure. Then we can use newtonian mechanics to calculate the development of the universe backwards from the present time.
"feature" size
<----->
● ● ● ●
● ● ● ●
o ~~~~~~ last scattering
| c = 1 / a
/\
observer
We set a = 1 as the current scale factor of the universe. In comoving coordinates, the speed of light
c ~ 1 / a.
Let us look at ten "epochs" where
a ≈ 1 / 2ⁿ,
0 ≤ n ≤ 10. The epoch 10 corresponds to the time of the last scattering, that is z ≈ 1,100.
In ΛCDM, the kinetic energy of a particle m in static (not co-moving coordinates) is very roughly
1/2 m v² ~ 1 / a = 2ⁿ.
That is, v ~ sqrt(2ⁿ).
This implies that the time the model spends in an epoch n is
t ~ (1 / 2ⁿ) / sqrt(2ⁿ).
The speed of light c ~ 1 / a = 2ⁿ. Light in that time propagates a distance in comoving coordinates:
Dₙ ~ 2ⁿ * (1 / 2ⁿ) * (1 / sqrt(2ⁿ))
= 1 / sqrt(2ⁿ).
We are interested in the distance
10
D = ∑ Dₙ
n = 0
in comoving coordinates, which light travels from the last scattering to the eye of the observer. The value of s forms a decreasing geometric series for n. If the contribution of epoch D₀ is 1, then the sum of the series is
D ~ 3.4.
In particular, the contribution of epoch D₁₀ is only 0.03. We see that we have to modify the physics drastically during epoch 10, if we want to increase D by 8%.
The first one billion years of the universe corresponds to a redshift z ~ 10. That is, the epochs 4, ..., 10 are relevant. The contribution D₄ = 0.25, and the the sum of D₄, ..., D₁₀ is 0.85. We see that if we modify physics substantially, but not drastically, during epochs 4, ..., 10, we can increase D by 8%.
*** WORK IN PROGRESS ***




