Dark Future for Dark Matter

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1. Introduction

The ΛCDM model is used to represent the expanding universe for the interpretation 1) of type Ia supernovae (SNe Ia) brightness and redshift data, and 2), of measurements of anisotropies in the cosmic microwave background (CMB) spectrum of the early universe. The model conjectures the existence of dark matter and dark energy—a lot of both. With a felicitous balance of the two, an ostensibly credible model is derived. However, a ΛCDM model has drawbacks. Firstly, the existence of dark matter is an unverified hypothesis.^{1} There have been numerous experiments dedicated to finding dark matter here on Earth, in underground experiments [2] [3] and satellite detectors [4], as well as in the Large Hadron Collider [5]. Yet, there has been no unambiguous dark matter detection [6], which, by induction [7], is evidence of absence. Moreover, aside from the ΛCDM model, there is no theoretical call for dark energy; nor has there even been an observational hint of its existence. Kang et al. [8] have recently challenged a key premise in the derivation of the ΛCDM model, and by addressing the problem with a different approach, we show that the model is utterly untenable. We expand, revise and interpret the Einstein field equation to find a simple viable alternative to the ΛCDM model.

2. Einstein Field Equation

We use the standard nomenclature of GR (e.g., see Kenyon [9] ), except k is the Newtonian gravitational constant and $c=1$ is the speed of light. The Einstein field equation is

${G}_{\mu \nu}=8\pi k{T}_{\mu \nu},$ (1)

where ${G}_{\mu \nu}$ is the Einstein tensor and ${T}_{\mu \nu}$ is the stress-energy tensor of a perfect fluid,

${T}_{\mu \nu}=\left\{\left\{\rho \mathrm{,}p\mathrm{,}p\mathrm{,}p\right\}\right\}\mathrm{,}$ (2)

where $\left\{\left\{\cdot \cdot \cdot \cdot \right\}\right\}\equiv \text{diag}\left[\cdot \cdot \cdot \cdot \right]$ , $\rho $ is the mass density, and p is the pressure (energy density).

The line element, $\text{d}{s}^{2}={g}_{\mu \nu}\text{d}{x}^{\mu}\text{d}{x}^{\nu}$ , reduces for the weak isotropic cosmic field, to ( [10], Eq. 10.84)

$\text{d}{s}^{2}=\left(1+2\varphi \right)\text{d}{t}^{2}-\left(1-2\varphi \right){\delta}_{ij}\text{d}{x}^{i}\text{d}{x}^{j}\mathrm{,}$ (3)

According to Einstein ( [11], p. 84), ${G}_{\mu \nu}$ “must be a differential tensor in the ${g}_{\mu \nu}$ that is completely determined by the following three conditions:

1) It may contain no differential coefficients of the ${g}_{\mu \nu}$ higher than the second.

2) It must be linear in these second differential coefficients.

3) Its divergence must vanish identically.”

For the nonce, let $\partial $ represent any partial derivative operator ${\partial}_{{x}^{\text{}i}}$ , and let g represent any component of ${g}_{\mu \nu}$ . According to the first two conditions, each component of ${G}_{\mu \nu}$ has the form $\partial g\text{\hspace{0.05em}}\partial g~\partial \varphi \partial \varphi $ or $g\text{\hspace{0.05em}}{\partial}^{2}g~\left(1-2\varphi \right){\partial}^{2}\varphi $ (… or zero). Then, to the first power in $\varphi $ , the only non-zero form of a ${G}_{\mu \nu}$ component is ${\partial}^{2}\varphi $ .

With
${G}_{00}=2\text{\hspace{0.05em}}{\partial}^{2}\varphi $ and
${T}_{00}=\rho $ , Equation (1) yields the Poisson equation. If any other
${G}_{\mu \nu}$ component, say G_{11}, is non-zero, then
${G}_{11}~{\partial}^{2}\varphi ={G}_{00}/2$ ; therefore
${T}_{11}~\rho $ , and
${G}_{11}\ne 0$ implies that
$p~\rho $ . With such an equation of state, the fluid is relativistic, which is to say that the characteristic thermal speed of the fluid is close to c, which it generally is not. The only viable alternative is to set G_{11} and all other terms of
${G}_{\mu \nu}$ except G_{00} equal to zero. But this requires that
$p=0$ , which is not generally true. We overcome this dilemma by adding
$8\pi k{g}_{\mu \nu}p$ to the RHS of Equation (1). Then both sides of

${G}_{\mu \nu}=8\pi k\left[{T}_{\mu \nu}+{g}_{\mu \nu}p\right]$ (4)

remain generally covariant and, with this essential correction, Equation (4) becomes

${G}_{\mu \nu}=\left\{\left\{2{\partial}^{2}\varphi \mathrm{,0,0,0}\right\}\right\}=8\pi k\left\{\left\{\varrho \mathrm{,0,0,0}\right\}\right\}\mathrm{,}$ (5)

where $\varrho =\rho +p$ . This is the full Poisson equation,

${\partial}^{2}\varphi =4\pi k\varrho \mathrm{,}$ (6)

which applies in all coordinate systems. It notably takes into account the gravitational charge equivalence of mass density
$\rho $ and energy density p [12];^{2} adapted to this nicety,
$\varphi $ is the Newtonian potential.

In general, the density does not need to be uniform. We can approximate the mass of the universe with an assemblage of point masses and consider just one point mass at a time. Then the Poisson equation for the potential due to one point mass M is ${\partial}^{2}\varphi =kM$ , and the Einstein field equation is a linear superposiition of Poisson equations.

3. The Expanding Universe

For a universe with vanishingly small $\varrho $ , the line element 3 reduces to

$\text{d}{s}^{2}=\text{d}{t}^{2}-{\delta}_{ij}\text{d}{x}^{i}\text{d}{x}^{j}\mathrm{.}$ (7)

Then ${G}_{\mu \nu}=0$ because this metric is independent of $\varphi $ ; GR obviously does not apply. But what if this nearly empty universe expands according to Hubble’s law? Then

$\text{d}{s}^{2}=\text{d}{t}^{2}-{\text{e}}^{2{H}_{0}t}{\delta}_{ij}\text{d}{x}^{i}\text{d}{x}^{j}\mathrm{,}$ (8)

so that
${G}_{\mu \nu}=3{H}_{0}^{2}{g}_{\mu \nu}$ , assuming that GR does apply.^{3} The Einstein field equation is
$3{H}_{0}^{2}{g}_{\mu \nu}=0$ , so
${H}_{0}=0$ . Clearly GR does not apply in this case either. However, we can force GR to apply by replacing the Einstein tensor
${G}_{\mu \nu}$ with its Lovelock [15] form
${G}_{\mu \nu}\to {G}_{\mu \nu}+b{g}_{\mu \nu}$ . Then the field equation is

$\left(3{H}_{0}^{2}+b\right){g}_{\mu \nu}=0.$ (9)

But b is merely an invention that allows us to broaden the scope of the field equation by allowing for Hubble expansion; it has no significance of its own. In fact, the Hubble expansion is real, but it is independent of GR.

Refashioned to try to accommodate Hubble expansion, Equation (5) becomes

${G}_{\mu \nu}+b{g}_{\mu \nu}=\left\{\left\{2{\partial}^{2}\varphi \mathrm{,0,0,0}\right\}\right\}+\Lambda {g}_{\mu \nu}=8\pi k\left\{\left\{\varrho \mathrm{,0,0,0}\right\}\right\}\mathrm{,}$ (10)

where $\Lambda =3{H}_{0}^{2}+b$ , which is zero according to Equation (9). There is no real change from Equation (5), but we use this form of the equation in Section 5, where Λ—there designated as the cosmological constant—is regarded as a proxy for dark energy.

4. The Coasting Universe

Evidence for the existence of dark matter is not at all conclusive. It is not needed to explain the flat rotation curves of spiral galaxies nor the CMB simulations. Concerning the rotation curves, alternate explanations have been published by Milgrom [16] [17], Brownstein and Moffat [18], Mannheim and O’Brien [19], Verlinde [20], ourselves [21], and others. As far as the CMB data are concerned, they show a compatibility with the ΛCDM model, but not that an equivalent compatibility is impossible for other models [22] [23] [24] [25]. Therefore if there is no dark matter $\varrho \approx {\rho}_{b}$ , the density of baryonic matter, whose value [26], ${\rho}_{b}\approx 3.6\times {10}^{-28}\text{kg}\cdot {\text{m}}^{-3}$ , is two orders of magnitude smaller than the critical density, ${\rho}_{c}=3{H}_{0}^{2}/8\pi k$ , so the gravitational forces and accelerations are negligible. Kolb [27] proposed such a linearly coasting universe, which Sethi et al. [28] found to agree “surprisingly” well with SNe Ia observations. Subsequently many others [29] - [58] have confirmed the validity of a coasting fit, which we now corroborate. The coasting universe expands without acceleration,

$a\left(t\right)=1+{H}_{0}t\mathrm{.}$ (11)

For redshift z, the distance between a source (then) and observer at $t=0$ (now) is

$r=\left(c/{H}_{0}\right)ln\left(1+z\right)\mathrm{.}$ (12)

The distance modulus depends on the area, $4\pi {f}^{2}$ , of the wavefront at $t=0$ . For an open universe [59],

$f=\frac{c}{{H}_{0}}\mathrm{sinh}\left[\mathrm{ln}\left(1+z\right)\right]=\frac{c}{2{H}_{0}}\left[1+z-\frac{1}{1+z}\right]$ (13)

is the luminosity distance.

In Figure 1, we plot a set of high-confidence Union 2.1 data [60]. We used these data to estimate
${H}_{0}=68.22\pm 1.00\text{km}\text{\hspace{0.05em}}\cdot \text{\hspace{0.05em}}{\text{s}}^{-1}\text{\hspace{0.05em}}\cdot \text{\hspace{0.05em}}{\text{Mpc}}^{-1}$ (
${\chi}^{2}=576.45$ ). It is the only parameter needed for calculating the superposed coasting curve. Because the number of degrees of freedom ν = 579 is large, the variable
$\xi =\left({\chi}^{2}-\nu \right)/\sqrt{2\nu}$ is approximately normally distributed with unit variance. For our solution,
$\xi =-0.075$ which, being a small value, substantiates the Union 2.1 observational error estimates as well as the coasting fit to the data.^{4} According to our
${H}_{0}$ , the age of the coasting universe is the Hubble time,
${H}_{0}^{-1}=14.33\pm 0.21\text{\hspace{0.17em}}\text{Gyr}$ . This is gratifyingly close to the 14.46 ± 0.31 Gyr age of HD 140283, the oldest star for which a reliable age has been determined [62].

5. The ΛCDM Model

Equating the $\mu \nu =00$ element pairs on both sides of Equation (10) gives

$2{\partial}^{2}\varphi +\Lambda =8\pi k\varrho \mathrm{,}$ (14)

whereas equating any of the $\mu \nu =\mathrm{11,22}$ or 33 element pairs gives

$\Lambda =0.$ (15)

Figure 1. Hubble diagram residuals for the linearly coasting model that best fits the Union 2.1 compilation set of 580 SNe Ia data points.

The ΛCDM model is based on Equation (14) (but while also implicitly ignoring Equation (15)). The first integral of Equation (14) is

$2\frac{\text{d}\varphi}{\text{d}r}=\frac{\left(8\pi k\varrho -\Lambda \right)r}{3}\mathrm{,}$ (16)

which, by Newton’s second law of motion, is

$\frac{{\text{d}}^{2}r}{\text{d}{t}^{2}}=\frac{r}{6}\left(\Lambda -8\pi k\varrho \right)\mathrm{.}$ (17)

With this choice, the ΛCDM scale factor for an expanding universe decelerates at first when $8\pi k\varrho >\Lambda $ , then later accelerates after $\Lambda >8\pi k\varrho $ ; the orthodox ΛCDM model does not expand at the same rate as the well substantiated linearly coasting universe that are discussed in Section 4. There is no way of formulating a linearly coasting universe with the ΛCDM model, so purported ΛCDM scale accelerations [60] [63] - [68] are then merely expected artifacts of the Equation (17) procrustean template. Anyway, according to Equation (9) of Section 3, and to the conventionally ignored Equation (15), the cosmological constant must be zero: the ΛCDM model should be rejected because it does not expand at all.

6. Conclusions

GR can be reconciled with a static universe by starting with the Einstein field equation (Equation (1)) if $p=0$ , or with the modified field equation (Equation (4)) if $p\ge 0$ . GR can also be reconciled with a uniformly expanding universe by replacing the Einstein tensor with its Lovelock form ${G}_{\mu \nu}\to {G}_{\mu \nu}+b{g}_{\mu \nu}$ . GR then turns out to be in full accord with the linear coasting universe determined from the collation of type Ia supernovae (SNe Ia) brightness and redshift data—without recourse to the existence of dark matter or dark energy.

The ΛCDM model requires the existence of vast quantities of (attractive) dark matter and (repulsive) dark energy. They are the sources of fanciful opposing forces that mostly cancel each other out. We have shown why this model must be wrong: according to Equation (15), $\Lambda =0$ . There can be no dark energy in the context of the ΛCDM approach, so this broadly accepted model is incorrect. Whereas dark energy is implausible and unnecessary, dark matter is not implausible and its need is unresolved. We recommend a linearly coasting universe—one that is consistent both with GR and with SNe Ia observations—as a viable ΛCDM alternative.

NOTES

^{1}Dark matter had a sullied reputation from the nineteenth century, when astronomers searched fruitlessly for another sort of invisible matter—an intramercurial planet, Vulcan [1], that was thought to be responsible for otherwise unexplainable orbital perturbations of Mercury. As it turned out, what had been missing was not matter, but an authoritative theory: GR. So, is it now missing matter, or missing theory?

^{2}Using an arbitrary equation of state for a perfect fluid, Peebles ( [11], Eq. 4.21) generalizes the RHS of Equation (6) to
$4\pi k\varrho \to 4\pi k\left(\rho +3p\right)$ instead of
$4\pi k\varrho \to 4\pi k\left(\rho +p\right)$ .

^{3}We derive this expression using L. Parker’s Mathematica [13] notebook, *Curvature and the Einstein Equation* [14], with only the following principal modifications:

^{4}With a three parameter (H_{0}, ρ, Λ) ΛCDM fit to the same Union 2.1 data, the Planck team [61] estimates H_{0} = 70 km∙s^{−}^{1}∙Mpc^{−}^{1}, χ^{2} = 545.11, and ξ = −0.939, which we view *per se *as reasonable because the magnitude of ξ, although larger than ours, is less than one standard deviation. (A smaller χ^{2} is not necessarily better in a χ^{2} test: the best fit occurs when χ^{2} = ν.) The qualities of the SNe Ia fits (ours and the Planck team’s) are commensurate, but the team’s ΛCDM model depends on the existence of an untenable fiction: dark energy.

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