On a more conceptual level we ask, along with some DM advocates, what is the point in astronomy and cosmology if they cannot be intimately linked with terrestrial-scale physics? Those two disciplines will forever remain limited to the passive collection of electromagnetic (and perhaps gravitational) waves from a single point-of-view. A deformation of terrestrial physics—which survived a plethora of active tests—experimentally inaccessible otherwise, is not really different from epicycles drawing and will always be achieved with enough of them—interpolation functions, additional fields and terms in the Lagrangian, etc.
The more pervasive view is that Einstein’s gravity should be kept, salvaged by new forms of yet unknown, exotic “dark matter” (“transparent matter” would have been more appropriate), at most weakly interacting with normal matter. This conjecture might seem too flexible to ever be refuted. Indeed, given , estimated on dynamical grounds, gravitational lensing, etc., a compatible e-m tensor is guaranteed to exist by Einstein’s equations. Representing dark-matter by with , the e-m tensor associated with directly observed baryonic matter, in conjunction with and at most weakly interacting (not via gravity) would always vindicate Einstein. Of course, should “balance” not only at some cosmological time but also throughout the entire history of the universe. However, given the speculative nature of that history, its highly indirect evidence, and the immunity granted to dark particles from being directly detected, dark matter does appear somewhat of a lazy solution.
The above, common criticism of the dark-matter conjecture ignores nonetheless a nontrivial observational fact: The energy density associated with is always found to be positive semi-definite, as expected of matter. Why should that be so if GR is wrong? In other words, why do we not also observe systems with too much mass rather than too little? Our proposal that is just the e-m tensor associated with the ZPF explains this critical point. It further trivially explains the transparency of “dark matter” to electromagnetic radiation (by the linearity of Maxwell’s equations). Finally, ordinary and (alleged) dark matter are observed clustered together, again, as if gravity does not discriminate between the two. This is explained in our model by the fact that the ZPF is just the sum of self-fields, each adjunct to an individual particle, declining with distance from it as must be the case for a radiation field. Regions rich in ordinary matter should therefore be also “ZPF rich”.
The analysis which follows relies on Equation (
22) for the fluctuations around the background. As in standard linearized gravity (See, e.g., [
10] Section 10.1 but note the different sign conventions for the metric) a subset of solutions to (
22) (with the last two term on its l.h.s. omitted) relevant to our case satisfies the simpler equation:
As
p still contains the fluctuations in the ZPF and the internals of atoms and molecules, both irrelevant to the dynamics of galaxies, we utilize the linearity of (
23) and “low-pass” it, viz. convolve it with a space-time kernel much wider than typical atomic size/time. Retaining the symbol for the low-passed
p, the resulting r.h.s. should be separately treated for matter and radiation dominated regions. Starting with the former, the following standard assumption is made regarding nonrelativistic matter:
. Only diagonal elements of
are therefore nonvanishing, the time-derivatives part of the l.h.s. of (
23) are obviously negligible for a slowly varying
p, and Poisson’s equation for the Newtonian gravitation potential,
, follows by defining
:
implying
.
4.1.1. Outline of a ZPF-Based Model of Dark-Matter
No attempt is made in this short section to fully cover the astronomical observations concerning dark matter which have been occupying telescopes around the globe for several decades. Instead, we shall demonstrate that any reasonable ZPF-based model of dark matter qualitatively captures the more universal aspects of this huge body of knowledge. It is crucial to understand that a full-fledged model cannot be derived from ECD alone for exactly the same reasons QM cannot. Both should be viewed as complimentary statistical theories to ECD, on equal footings with the latter. As with QM, simplicity criteria can be postulated such that the model becomes the simplest, perhaps unique such compatible statistical theory, but the postulates themselves would obviously not be derivable from ECD.
According to our proposal, rather than inventing new forms of matter to explain the apparent deficit on the r.h.s. of (
24), one has to take into account the effect which ordinary matter has on its surrounding ZPF. Consequently our missing “transparent component” of
has several nonvanishing components besides
, clearly distinguishing it from ordinary cold dark matter—see
Section 4.1.4.
The transparent
will be estimated from the paths,
of all relevant particles, labeled by
a. Only their dipole fields will be used to represent their radiation (the Coulomb part, by our previous remarks, appears in the e-m of matter), but this is just to ease the presentation, with higher order multipoles adding nothing essentially new to the analysis. In this approximation, we have
and (
26) is to be evaluated at the retarded/advanced time, defined by solutions to
Above,
and
are the associated magnetic and electric fields;
is its c.o.m.; and
is a unit vector pointing from it at the point of interest,
. The particle’s effective dipole moment is
with
as its charge density and “dot” standing for a time derivative.
The derived low-passed (see the following (
23)) electromagnetic energy density,
involves both a double summation (
26) over the particle labels and a separate count for their advanced and retarded contributions. It is clearly still time-dependent, but we shall only consider systems for which this time dependence can reasonably be assumed to be negligibly slow. As the time-averaged masses of the particles are assumed to be constant, the retarded and advanced contributions are equally weighted, reflecting
in (
10). Strictly speaking, equally weighting retarded and advanced contributions is wrong, as the decomposition (
15) implies. However, insofar as the last term in (
15)—that associated with the ZPF—when integrated over scales of an entire galaxy is on the order of the galaxy’s baryonic mass, the first term—that associated with macroscopic retarded radiation—and hence also the second term, can both be easily shown to be negligibly small in comparison.
The remaining components of
will only interest us in
Section 4.1.4, dealing with gravitational-lensing tests of dark matter. Qualitatively, they are as follows. Far from a dipole, the local radiation field is well approximated by a sum of plane waves, each of the form
for some
f, with an associated canonical tensor
. Advanced and retarded contributions of each dipole to the local ZPF have opposite signs for their
s but the same for their
s. Since the ZPF receives nearly balanced contributions from retarded and advanced fields (
Figure 2), the Poynting vector
is negligible compared with
and
.
Had all dipoles been independently radiating, only “diagonal terms” in (
28), viz.
in (
26), would have contributed, resulting in a trivial sum of “
halos” centered at every dipole. Not only would that render the “Friedman DC”,
, infinite, but also it would further contradict the high degree of interparticle connections, discussed in
Section 2.3 and in the context of our classical photon model (
Section 3.1.4). Such interconnectedness mandates a certain degree of statistical dependence between any two dipoles at the intersection of their world-line with the other’s light-cone. A premise of any consistent model must therefore be that this statistical dependence is destructive, viz. results in a (statistically) negative contribution to (
28).
The destructive interference we refer to above is similar to the classical process of absorption discussed in
Section 3.1.4, dealing with photons, but with one critical difference: There, the destructive interference between the incident retarded field and the secondary retarded field, generated by the absorbing system, entails the excitation of that system in order to respect energy-momentum (e-m) conservation. In the current case, the incident retarded field superposes destructively also with the advanced field of the absorbing system (see
Figure 3). This destructive interference guaranties that the Poynting flux across a sphere,
S, containing the absorbing system (or, as it should more appropriately be called in this case: the reacting system), vanishes, respecting its equilibrium with the ZPF. Reversing the roles of advanced and retarded fields, the advanced field of system b is likewise absorbed by system a. At the level of equilibrium with the ZPF, the arrow-of-time is inconsequential.
Which dipole pairs are candidates for such destructive correlations? The interconnectedness of all dipoles notwithstanding, any realistic model can safely neglect all pairs,
, other than those for which
,
and
are approximately collinear. Otherwise, their correlation would necessitate at least a third dipole,
c, whose world-line intersects the intersection of
a’s and
b’s light-cones—a circle at a constant-time slice. Not only is that improbable (zero probability for point dipoles) but it would also be “second order” in a typical inter dipole correlation strength. Now, the probability of a random
being collinear with any pair
is also zero. However, for any pair, there exists an entire line,
, satisfying the collinearity condition. It is along such lines, any model must assume, that destructive interference occurs. Now, for
n dipoles there are
pairs (whose negative contributions to the energy density (
28) are clearly interdependent, decreasing with
n on average if only to guarantee (
28)’s positivity). In conjunction with the diminishing distance-dependence of that interference (as explained in the caption of
Figure 3), it follows that, for a given volume,
V, hosting the dipoles, the average interference increases with increasing
n and decreasing
V, or equivalently
Consider next a highly inhomogeneous distribution of dipoles comprising a relatively dense “nebula”,
, embedded in a tenuous background,
. Assuming that the contribution to the energy density (
28) coming from background pairs
is effectively
-independent in the (large) neighborhood of
due to large numbers and sparsity of
, and that contributions of mixed pairs,
are negligible in that neighborhood (by the remarks made in the caption of
Figure 3), one is left with nebula pairs of only
, responsible for the ZPF’s contribution to
. For a nebula in which the center coincides with the origin and for
, viz. away from the nebula, we can Taylor expand (
26) in powers of
, resulting in a (typically non-spherically symmetric) transparent “halo” (
28):
For sufficiently large
, the assumptions underpinning (
30) collapse and
merges seamlessly with the uniform coarse grained background
, rendering the energy of the halo finite. This facilitates the calculation of its generated gravitational potential,
(
24), using the standard Green’s function of the Laplacian (which assumes a vanishing potential at infinity):
with
the angle between
and the direction of the spatial angle
. The upper integration limit,
, guaranteeing the finiteness of the integral, is a convenient substitute for the actual, integrable large
tail of the halo. The result of (
32) is
The gradient of
at
is entirely dominated by the lower integration limit, and is further independent of
. It has a radial component
which is just the force field generated by a standard (spherically symmetric) isothermal halo and a transverse component, viz. orthogonal to
(unless the ZPF halo (
30) is spherically symmetric) similarly decaying as
. For the important case of a disc nebula, the transverse component vanishes in the disc’s plane (by simple symmetry arguments).
The constant C above, being an average over ’s “transmittance”, , in all directions, is some global attribute of the nebula, already depending on more specific details of a model. However, in any reasonable model, we would have the following:
(a) The constant
C increases with increasing average strength of dipoles comprising
. Reviewing
Section 3 in this regard, it is reasonable to anticipate that the main source of the halo (
30) is radiation linked with the bulk acceleration of electrons. Indeed, for a particle to have a strong radiation field, it must have a large/rapidly varying effective dipole (
27). Freely moving particles, by their minute size and conserved charge, have tiny multipoles (in their c.o.m. frame), while their scale equilibrium entails that the fluctuations of their
in (
10) around their mean,
, are relatively small. This implies that significant bulk acceleration is a necessary condition, hence the dominance of electrons, which are by far the lightest among the stable particles.
Rapid bulk acceleration occurs whenever the free motion of a charge is perturbed by a rapidly varying potential. This clearly is the case for ECD electrons bound in atoms and molecules, but any sufficiently dense environment also guarantees such conditions. As most baryons in the current epoch are in the form of tenuous plasma, in which electrons are freely moving for many years between collisions, major ZPF sources can only be neutral galactic gas and stars (the latter, despite being plasma dominated, are some thirty orders of magnitude denser than the intergalactic medium). This conclusion is further consistent with the results of [
6], where a lower bound,
, was calculated for the ratio between the current average energy density of baryonic matter to that of the ZPF. Had the intergalactic medium generated ZPF in a proportion to its mass, on par with that of galaxies,
would have had to be much smaller.
Correlating with the number of electrons in a nebula, the constant
C in (
34) also correlates with the nebula’s mass, the reason being the dominance of Hydrogen (and Helium to a lesser extent) and the overall neutrality of baryonic matter.
(b) By point
29, for a fixed dipole strength and nebula’s geometry,
C’s dependence on the number of dipoles,
n, is concave, as larger
n imply larger negative-energy cross-terms per dipole in (
28). This is clearly true also for the ZPF intensity inside
or in its immediate neighborhood. A natural such concave dependence would satisfy
To wit, the contribution of an added dipole to the halo energy density (
30) is (statistically) suppressed by exactly the already present energy density interfering with it, which is proportional to
C.
4.1.2. Spiral Galaxies
The best laboratories for testing dark-matter theories are spiral (or disk) galaxies. Matter in the disk’s plane circles the galactic center at a speed which depends only on its distance from the galactic center—a dependence known as a rotation curve. This makes spirals the only astronomical objects in which the local acceleration vector of moving matter can be reliably inferred from the projection of their velocity on the line-of-sight, as deduced from the Doppler shift of their emitted spectral lines.
One universal feature of rotation curves concerns the radius beyond which they begin to significantly deviate from the Newtonian curve, viz. that which is calculated based on GR + baryonic matter [
11]. This happens at around a radius at which the radial acceleration of orbiting matter equals some universal (small) value,
, known as the MOND acceleration. That such behavior, having no plausible explanation within the dark-matter paradigm, is expected from our model, followed by first asking: Where should “ZPF dark matter” kick-in? Point (
29) implies that the energy content of the disc near its dense center is baryon-dominated until a critical radius,
, beyond which its surface density drops below some critical value
, and this conclusion is independent of the exact interference model which can only affect
’s value and the transition region,
. For the same reason, the halo’s intensity inside a sphere of radius
, co-centered with the disc, is much smaller than implied by (
30). It follows that, under the approximation wherein the sphere’s entire mass content is “moved” to its center, the rotation curve should be approximately Newtonian for
. Now, given that the coarse grained surface density of any spiral can be fitted rather well using only two parameters
it can then be shown by a straightforward calculation that the radial acceleration at
takes the form
for a slowly varying function
, approximately equal to 1 on
(as is the case for
x in most spirals). The MOND result follows upon defining
.
Moving beyond
in the galactic plane, the rotation curve eventually flattens, as follows from the asymptotic gradient, (
34) (the contributions of baryonic matter and of small
corrections to (
30), both drop faster, as
). The square of that asymptotic (tangential) speed correlates rather well with
and the total mass,
M, of the galaxy and reads
. This relation, also known as the Baryonic Tully–Fisher relation (BTFR), is also compatible with our model simply on dimensional grounds. As
is a solution of (
24), the
C appearing in (
34) must have dimensions
. We further want it to monotonically increase with
and with
—both increasing with the number of radiating dipoles. In the latter case,
C’s dependence should be concave, as more particles also imply greater cross-term destructive interference. Finally,
C should monotonically increase also with
. A larger
implies smaller interference effects, meaning that more radiation escapes the galaxy (note, again that
already incorporates the details of any reasonable interference model). The obvious candidate up to a dimensionless coefficient is
, rendering the full coefficient of the gradient (
34)
, which is the BTFR. Note that, as
M is proportional to
n, the number of dipoles contributing to
C, the above choice conforms with (
35). The dimensionless coefficient can only be a function of the ratio
. The above conditions on both
’s imply that this function is slowly varying and, moreover, of an argument belonging to a relatively short interval.
An apparent weakness in the above analysis is that MOND’s independence on the spiral’s composition is not readily explained. It is not entirely clear why, e.g., a frenetic electron in a star’s core should, on average, contribute to the ZPF on par with a bound hydrogen electron in a gas-dominated spiral, given their vastly different bulk motions. This composition independence suggests that it is not directly bulk acceleration which is responsible for the ZPF but, instead, the accompanying fluctuations in an electron’s morphology and associated
. In other words, the ZPF is a manifestation of energy exchange between electrons which are temporarily out of scale equilibrium. In light of the properties of the ZPF discussed in
Section 2.3, it is rather natural for all electrons actively participating in such redistribution of energy to contribute, on average, similar amounts.
Summarizing, the MOND phenomenology, attributing a fundamental significance to , appears as a deceiving coincidence between the relatively large ZPF contribution to the mass in sparse regions of a galaxy and the small Newtonian acceleration there. Besides in spirals, this coincidence manifests itself also in dwarf spheroidals and other, low-density pressure-supported systems.
4.1.3. Clusters of Galaxies
When dealing with the dynamics of galaxies in a cluster, the upper cutoff
in (
32) can no longer be arbitrary and must represent the physical radius, around which a galaxy’s ZPF halo merges with the Friedman ZPF DC, rendering the galaxy’s mass finite. In sufficiently sparse clusters, the halo size can reasonably be assumed to be much smaller than the average intergalactic distance; hence, in the Newtonian approximation, each galaxy can be modeled by a point in which
gravitational mass comes mainly from its halo.
What about a galaxy’s
inertial mass? The geodesic equation, even in its Newtonian approximation (
25), is of course oblivious to this question, and a galaxy should move in the field of all others independently of that extra ZPF energy it carries. Nonetheless, if we wish to make full use of Newtonian gravity and, in particular, its expression for the conserved e-m, the halo must be treated as if also contributing to a galaxy’s inertial mass. When doing so, the virial theorem is a legitimate tool for estimating the contribution of ZPF halos to a cluster’s mass (The alert reader may ponder whether this extra inertial mass is consequential to electromagnetic interaction between particles. The answer is negative, as is evident from the derivation of the Lorenz force equation in appendix D of [
1]).
The flat rotation curve of spirals typically persists to the observational limit, which could be at ten times a galaxy’s optical diameter or even beyond. It is therefore unclear which clusters qualify as “sufficiently sparse” and, consequently, whether the virial theorem is a legitimate tool for estimating their mass. From the above lower bound on a galaxy’s halo size, it is however clear that, in some clusters or at least in the central regions thereof, a typical halo size certainly exceeds intergalactic separation distance. In such cases, two complications arise. First, as the halos are typically not spherically symmetric, the point-mass approximation collapses. Second, the hitherto ignored interference cross-terms between dipoles belonging to distinct galaxies must be taken into consideration. Specifically, as relativistic e-m must be conserved, the electromagnetic e-m subtracted from two halos approaching each other as a result of such destructive interference must appear elsewhere, such as in the bulk motion of galaxies or in the intracluster medium.
There is, nonetheless, a good indication that naively “attaching a fixed halo” to each galaxy is a decent first approximation. Most of a cluster’s baryonic mass (90–80%) comes from the Intracluster Medium (ICM)—a tenuous plasma of average mean-free-path
light-year. The gravitational potential in the cluster can be inferred from the density and temperature distributions of the ICM [
12]. From that potential, one can determine (via Poisson’s equation) the sourcing mass distribution which, as predicted, is found to be dominated by some “phantom mass” for which the distribution follows rather closely that of galaxies rather than of the ICM. As a bonus, this result provides a confirmation for our model’s prediction that tenuous plasma contributes only little to the ZPF.
4.1.4. Gravitaional Lensing
An apparent independent confirmation for the last point above, comes from the so-called “Bullet Cluster” (1E 0657-558), whose alleged collision with another cluster had stripped both from their ICM, leaving two clusters composed virtually of galaxies only. Although the mass of the plasma left behind greatly exceeds that of the bare clusters, the total mass distribution in the region of collision, as inferred from weak gravitational lensing of background galaxies, is dominated by phantom mass whose distribution correlates well with the distribution of galaxies alone [
13] (Abell 2744—Pandora’s Cluster—is yet another good example). Nevertheless, our putative electromagnetic dark matter differs from ordinary cold dark matter in many respects. Inferring
from lensed images of background objects might yield erroneous results if our model is in fact valid—hence a questionable confirmation.
Conventional gravitational lensing calculations are all based on null geodesics in the following degenerate metric:
where
is sourced by
of both dark and ordinary, nonrelativistic matter. The source
cannot be uniquely deduced from the image, and various additional assumptions are needed for that, e.g., spherical DM halo in the case of single galaxies. This is one place where our model departs from CDM (cf.
Section 4.1.1). Even more critically, in our model
for the dark-matter part of the e-m tensor and, consequently,
, invalidating (
37).
It might appear that the addition of six extra “dark components”,
, to the (symmetric) e-m tensor has rendered our model too flexible to be refuted by any observation, but this impression is wrong. From
, the trace of the so-called Maxwell stress,
, must equal
, while
and
implies
. Moreover, exactly the same destructive interference affecting
(
Section 4.1.1) also affects
and, given a detailed (reasonable) interference model,
would essentially be uniquely determined by
. For example, the nebula’s halo analyzed in
Section 4.1.1 must have
for large
, on the above grounds only, implying
. The deflection angle of a light-ray traveling in the outskirts of a spherically symmetric halo is
smaller in our model than in a CDM (isothermal) halo having the same effective
(recall the factor 2 relative to (
24)). Gravitational lensing, especially strong lensing by non-isotropic halos, is therefore an excellent laboratory for confronting our model with standard CDM.