An uniform model for Dark Matter and Dark Energy

In this paper, after reviewing some of the most important concepts about Dark Matter and methods of its registration, in particular by using SQUIDs, a toy uniform model for Dark Matter and Dark Energy is proposed. In the frame of the model Dark Matter particles is interpreted as excitations of Dark Energy field. The devices based on SQUID, in particular the SQUIDparamagnetic absorber and the SQUID-magnetostrictor systems, both suitable for investigations of above problems, are considered. Estimates, is carried out within this model, indicate the possibility of experimental detection of the "ether wind" pressure, created by the non-corpuscular incoming flow, corresponding to the galactic orbital motion of the Earth.


Introduction
The nature of dark matter (DM) is one of the most urgent unsolved problems in modern physics, so physicists persistently try to find signs of elusive dark matter that tugs on everything but emits no light. History of observations and theoretical arguments for the DM existence are described in a recent review [1]. Besides large number of independent astrophysical and cosmological observations, such as galaxy rotation curves [2], large structure formation [3], and the observed spectrum of the cosmic microwave background [4,5,6], indicates that about 26% of the total mass-energy of the Universe is non-baryonic and non-relativistic cold component, which is not subject to electromagnetic interactions. Despite the long history of observations the particle content of DM remains unknown [7,8,9]. One possible solution would be the existence of new particles beyond the Standard Model. Among many candidates for DM particles the most favored are the so-called WIMPs (weakly interacting massive particles) with a mass in the GeV to TeV range [10,11]. The WIMPs existences are well motivated, as provide solutions for outstanding issues in both cosmology and particle physics. These particles appear in extensions to the Standard Model such as supersymmetry with R-parity conservation, and freeze out in the early Universe with an abundance that matches cosmological observations. Now DM particles can be detected in the laboratory experiments via elastic scattering off nuclei, causing recoils of a few keV in energy.
However, no experimental indication for a standard WIMP was found in high sensitivity direct search experiments like EDELWEISS [12], XENON100 [13], LUX [14], SuperCDMS [15] for more than a few tens of GeV/c 2 mass.
Thermal relics with masse below 100 GeV/c 2 are also disfavored both from constraints set by Fermi-LAT searches for annihilation signals from Milky Way dwarf galaxies [16], and from the impact that WIMP annihilation would leave on the cosmic microwave background anisotropies [17]. Furthermore search for dark matter particles directly produced in protonproton collisions in the CERN LHC experiments ATLAS and CMS did not show any indications of such particles so far [18,19,20].
On the other hand in the region of light WIMPs below 30 GeV/c 2 , some experiments such as DAMA/LIBRA [21], CoGeNT [22], CRESST [23], CDMS II Si [24] claim or are interpreted as finding dark matter signals.
It is obvious that for observation of low-energy WIMP-induced nuclear recoils, detectors with both low detection threshold and a very low background are needed. The sensitivity of a dark matter direct detection experiment depends on the WIMP mass and on the nature and strength of its coupling to atomic nuclei.
Alternative to the quest of WIMP particles is a search of ultralight DM particles such as neutrino, dark photons or axions. Again, there is no indication that the high-energy neutrinos originating from dark matter annihilations in the Sun, which can escape and be observed by neutrino telescopes, such as Baksan [25], Super-Kamiokande [26], ANTARES [27] and IceCube [28].
When arguing the existence of Dark Matter (DM), which exceeds the mass of the visible Universe by about five times, with the help of light particles, the component can be light, weakly interacting, pseudoscalar bosons -axions (ma ~ 1÷1000 μeV) [29].
Axions were introduced as a consequence of an extension of the Standard Model. The expansion, in particular, follows from the desire to preserve CP invariance, which is violated by the absence of an electric dipole moment in the proton, and axions, as particles of a new field that preserves CP invariance, play this role [30][31][32]. Moreover, new particles have no charge. Unexpectedly, it turned out that astrophysical and cosmological problems of the energy balance when calculating the emission budget of stars, the existence of halos around galaxies [33,34], the cooling processes of white dwarfs [35], and the shortening of the duration of the SN 1987A supernova explosion [36,37] can also be described more simply, using the existence of axions. (According to estimates [29,37], the particle density is ~ 10 21 m -3 ). Thus, the axions that make up the DM can be detected not only at accelerators, but also in laboratories studying cosmic radiation, since it serves as a source of axions [38,39].
The mechanism of the conversion of an axion into two photons in an external magnetic field (Primakov's mechanism), proposed earlier to explain the decay of muons, was chosen as a mechanism convenient for registering axions [40]. The reverse process of transformation of photons into axions is also possible. In addition, in the laboratory it is possible to use sources of powerful coherent radiation (lasers) and with their help simulate the conversion of photons into axions, as well as the reverse process. An additional impetus to research on the conditions for observing axions was the applied problem of detecting the passage of an axion beam through the thickness of matter without a significant weakening of its intensity -the LSTW (light shining through walls) experiment [41]. It was proposed to use a small interaction cross section to establish communication through massive opaque obstacles, for example, the Earth or Earth -Moon.
As noted above, the Primakov's mechanism uses low-frequency virtual photons of the magnetic field that resonate with the field of axions. The probability of the axion-photon conversion is p ~ (gB0l) 2 -here g is the constant of the photon-axion coupling. Strong enough magnetic fields B0 (B0~10 2 T ) along the entire path l (~10 2 m), where the conversion takes place as well as intense laser beams (~10 21 W/cm 2 ) for such reactions are required [42] . Because during solar flares on Sun surface there are a lot of photons piercing magnetic field, then it is possible to observe axion generation by helioscope (IAXO project) [43].
In recent time some investigators expect the time intervals measurements are keys for DM observation [44,45].  [46]. The long-scale structure depends on a matter density, the CMB anisotropy -defines by fluctuations of a cosmological gravitational potential, which changes the photon frequency. The effect is in a good agreement with the prediction of the concordance ΛCDM cosmology [47][48][49].
According to an offered model, with DE density of about 300 TeV/m 3 , it represents the unperturbed state of "Dark Substance", while its folds or perturbations play the role of elementary DM heavy particles. These particles will be stable if all their decay channels into any combination of other particles are blocked, or also, in our case, if their potential will have local minima, i.e., local traps providing metastable excited states. The Hamiltonian with metastable traps can be represented, for example, as follows: The nonlinear wave equation, corresponding to this Hamiltonian, and describing the dynamics of perturbations to Dark Substance will be like the "quasi-sine-Gordon" equation ( Moreover, the nonlinear potential (1), has the analytic structure very similar to the "parabolic washboard potential" [50] used to describe metastable states in the superconducting ring of a SQUID with one Josephson junction, namely: where Φ is the magnetic flux piercing the superconducting ring and L is the inductance of the circuit itself. We represent the profile of the washboard potential in figure 1.  In order to register such pressure, a dynamometer that performance capable to fix the strength of 10 -16 N at the end of the cylinder, which dimensions ℓ×S ≈ 1m×0.15 m 2 , is required. Apparently, the suitable candidate for the role of the super-high-sensitivity dynamometer is the SQUIDmagnetostrictor system [53][54][55] which has been previously supposed to be used in projects for the detection of gravitational waves, etc. (Figure 2).

Fig 2.
Schematic view of the SQUID-magnetostrictor system for the detection of gravitational waves (the magnetostrictive cylinder is represented in grey) [55].
Ultra-high sensitivity is achieved by means of this system. In fact, high strain-gauge effectiveness of the sensor can be achieved, since it operates on the principle of the reverse magnetostrictive effect, generated, in its turn, by collective quantum solid-state effects [61]. On the other hand, the high ("quantum scale" level) sensitivity of SQUID systems, used as measuring instruments, allows accurate registration of events.
The physical quantity describing the reverse magnetostrictive effect (discovered by Emilio Villari in 1865) in a particular material is the ratio of the internal magnetic induction field to the growth of its outside pressure, i.e., P . For example, an alloy made up of 54% Pt and 46% Fe, with μ ≈14000, will have Λ (-1) ≈10 -4 T / Pa (which is basically not a record value). Thus the magnetic response, measured by the SQUID, is related to the force action δF by this expression δΦ=Λ (-1) δF. Accordingly, the capability to register the pressure of non-corpuscular Dark Matter flow, estimated above for σ ≈ 2 35 10 cm  at δF ≈ 10 -16 N, requires an "absolute" (not reduced to the time of the signal accumulation) SQUID sensitivity for the magnetic flux of the order of magnitude of 10 -20 Wb ≈5×10 -6 Φ0. The actual value of a good DC-SQUID is of about δΦ ≈ 10 -6 Φ0/√Hz, which provides the desired sensitivity with a margin of approximately 2 orders of magnitude (at least) due to the possibility of a 3-hour signal accumulation.

Conclusions
In this paper, starting from an introduction about DM and its cosmological properties, we have focused our attention on a brief description of a toy model unifying DE and heavy DM component. In the context of "unifying" trend, clearly dominant in the modern elementary particle physics, we have also proposed a simple unimodel, where we try to consider the corpuscular Dark Matter (DM) and non-corpuscular Dark Energy (DE) from single approach.
This is the proposed model, in which the DE is an absolutely continuous substance, playing the role of a room for metastable excitations, which can be identified as Dark Matter particles.
From this point of view, we cannot assume DE as a medium suitable for the role of absolute spacetime, relative to which the states of other objects are considered. DE is rather an active medium, one of the manifestations of the activity of which is the effect of the production of DM particles.
The dual form of the DE entity gives possibilities for experimental research. Estimates, carried out within that model, indicate the possibility of detection of the "ether wind" pressure, created by the non-corpuscular incoming flow, corresponding to the galactic orbital motion of the Earth. It is argued that these types of investigations could be performed by using the SQUIDmagnetostrictor experimental system. At the same time, the concept of quantizing the continuity of the medium, which was used in the article, should undergo some modification in order to establish the boundaries of possible quantization both in the energy scale and in the spatial one.