Holography, Charge, and Baryon Asymmetry ()

T. R. Mongan

84 Marin Avenue, Sausalito, CA 94965 USA.

**DOI: **10.4236/jmp.2012.37079
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84 Marin Avenue, Sausalito, CA 94965 USA.

The reason for baryon asymmetry in our universe has been an open question for many years. This note shows that the holographic principle *requires* a charged preon model underlying the Standard Model of particle physics and, in consequence, *requires* baryon asymmetry. The baryon asymmetry predicted by a specific charged preon model in our closed inflationary Friedmann universe is consistent with observations.

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T. Mongan, "Holography, Charge, and Baryon Asymmetry," *Journal of Modern Physics*, Vol. 3 No. 7, 2012, pp. 581-584. doi: 10.4236/jmp.2012.37079.

1. Introduction

The reason for the dominance of matter over antimatter in our universe has been a relevant issue for years [1]. Several complicated mechanisms have been proposed to account for baryon asymmetry (matter dominance), but they all require new particles or phenomena that have not been observed. In contrast, this note shows that the holographic principle [2] provides a simple mechanism requiring baryon asymmetry The holographic principle, developed from black hole thermodynamics, says all physics at a given point is described by the finite number of bits of information on the particle horizon at the greatest distance from which a light signal could reach the point since the end of inflation. There is a temperature associated with the particle horizon and thermodynamics on the horizon implies gravity is explained by Einstein’s theory of general relativity [3,4].

The outline of this note is straightforward. First, after a brief discussion of the holographic principle, it is pointed out that the finite number of bits of information allowed by the holographic principle necessitates a charged preon model underlying the continuous mathematics of the Standard Model of particle physics. Second, it is noted that the holographic principle states that events within the universe are specified by the information on the particle horizon, and the characteristics of the particle horizon at the time of baryogenesis are determined. Third, it is shown that thermodynamics on the particle horizon at the time of baryogenesis requires baryon asymmetry. Finally, the results are compared with observations and it is noted that a similar analysis requires a lepton asymmetry resulting in a positron excess in the universe.

2. The Holographic Principle

The holographic principle says all information available about physics within a horizon at distance from an observer is given by the finite amount of information on the horizon. The number of bits of information on the horizon, specified by one quarter of the horizon area in Planck units [2], is. The Planck length, where

cm^{3}/g∙sec^{2},

g∙cm^{2}/sec, and cm/sec. The following analysis relies on Bousso’s [2] formulation of the holographic principle in terms of the light sheets of the causal horizon, circumventing earlier objections [5-7] to using the holographic principle in cosmological contexts. In particular, the argument applies to a vacuumdominated closed universe, created spontaneously by a quantum fluctuation, that can never collapse [8].

Because it involves continuum mathematics, the Standard Model can only approximate an underlying finite-dimensional holographic theory. In particular, a finite dimensional model involving only bits of information on the horizon must describe all physics occurring within the horizon. Linking bits of information on the horizon with Standard Model particles requires a holographic model describing constituents (preons) of Standard Model particles in terms of bits of information on the horizon.

3. Holography Requires Charged Preons

All Standard Model particles have charges 0, 1/3, 2/3, or 1 in units of the electron charge, so bits in a preon model must be identified with fractional electric charge. Furthermore, in any physical system, energy must be transferred to change information in a bit from one state to another. Labelling the low energy state of a bit and the high energy state (where is some non-zero integer depending on the particular preon model chosen) then amounts to defining electric charge. If the universe is charge neutral (as it must be if it began by a spontaneous quantum fluctuation from nothing) there must be equal numbers of and charges. A holographic charged preon model in such a universe then embodies charge conservation, a precondition for gauge invariance and Maxwell’s equations.

Protons have charge and anti-protons have charge Therefore, regardless of the details of how bits of information on the horizon specify a proton or antiproton, the preon configuration specifying a proton must differ in bits from the configuration specifying an anti-proton. Then, because bits and bits do not have the same energy, the number of protons and anti-protons created in the early universe must be slightly different. In other words, if bits have lower energy than bits, there will inevitably be more matter than anti-matter in the universe. However, a small difference in energy of the bits on the horizon specifying a proton or anti-proton is not inconsistent with protons and anti-protons having identical mass.

4. Particle Horizon at Baryogenesis

The temperature at the time of baryon formation was ˚K, where the Boltzmann constant (g∙cm^{2}/sec^{2})/˚K, and the proton mass g. So, the scale factor of the universe at the time of baryogenesis was [9,10] cm, where 2.725 ˚K is today’s cosmic microwave background temperature and the scale factor of the universe today is cm. The time of baryogenesis, in seconds after the end of inflation, can be determined from the Friedmann equation . After inflation, the universe is so large it is almost flat, so the curvature parameter. The energy density is , where, , and are, respectively, today’s radiation, matter, and vacuum energy densities. Since the radiation energy density [11] erg/cm^{3}, the matter energy density erg/cm^{3}, and vacuum energy density was negligible in the early post-inflationary universe, the radiation term dominated when, before radiation/matter equality. Integrating , where , from the end of inflation at to gives, where is the scale factor of the universe at the end of inflation. Therefore, seconds, if. The distance from any point in the universe to the particle horizon for that point [12] is

Since, cm.

5. Thermodynamics on the Event Horizon

The surface gravity on the particle horizon at baryogenesis is, so the associated horizon temperature [3] is ˚K. The temperature at any epoch is uniform throughout a post-inflationary homogeneous isotropic Friedmann universe, and the causal horizon at baryogenesis is at distance from every point in the universe. The temperature at every point on the causal horizon for every point in the universe is the same because the surface gravity of the uniform sphere within the horizon is the same at every point on every horizon. The bits on all causal horizons are in thermal equilibrium, and there are only two quantum states accessible to those bits. Therefore, the use of equilibrium statistical mechanics is justified and the occupation probabilities of the two bit states in thermal equilibrium at temperature are proportional to their corresponding Boltzmann factors. So, if the energy of an bit on the horizon at the time of baryon formation is and the energy of a bit is, the proton/antiproton ratio at baryogenesis is. Since , the proton excess is.

6. Holography Requires Baryon Asymmetry

Any holographic preon model must link bits of information on the horizon to bits of information specifying the location of preon constituents of Standard Model particles within the universe. The wavefunction specifying the probability distribution for the location of a particular bit of information within the universe has only two energy levels. The energy released when a bit in the universe drops from the (1) to the (0) state raises another bit from the (0) to the (1) state, and that is the mechanism for charge conservation. The energy must be transferred by a massless quantum with wavelength related to the size of the universe. There is no reliable definition of the size (as opposed to the scale factor) of a flat or open universe, so it is necessary to restrict the analysis to closed Friedmann universes. The only macroscopic length characteristic of the size of a closed Friedmann universe with radius (scale factor) is the circumference. If the energy to change the state of a bit associated with a preon within the universe (and the corresponding bit on the horizon) at baryogenesis equals the energy of massless quanta with wavelength characteristic of the size of a closed Friedmann universe with radius,. Then, substituting from above, the proton excess at baryogenesis is . The dependence on arises because, the radius of the universe at baryogenesis, depends on, today’s cosmic microwave background temperature 2.725 ˚K, and the temperature at baryogenesis. For cm, the proton excess is.

7. Comparison with Observations

The WMAP estimate [13] of baryon density to cosmic microwave background photon density ratio is . A charged preon model [14] with involves three strands, with charged bits on the end of each strand, bound by non-local forces into each Standard Model particle. At the time of baryogenesis, the number of proton states with six bits, the number of antiprotons states with six bits, and the number of photon states with three and three bits are approximately equal. Then, when almost all protons and anti-protons annihilate to two photons, the ratio of baryon to photon states is, in good agreement with the WMAP result.

8. Holography Requires Positron Excess

Replacing the proton mass with the electron mass in the above analysis predicts a positron excess of when the universe cools to the point where electron-positron pairs can survive. This primordial positron excess constitutes a primary source of positrons that might help explain cosmic ray positron excess in the PAMELA experiment [15,16]. The positron excess might also explain part of the asymmetric 511 keV gamma radiation from the galactic center [17].

9. Conclusion

The holographic principle requires a charged preon model underlying the Standard Model of elementary particles and, in consequence, requires baryon asymmetry. So, in charged preon models, thermodynamics on the particle horizon requires baryon asymmetry, and the baryon asymmetry estimated for a closed universe is consistent with observations. This simple explanation for baryon asymmetry suggests baryon asymmetry and the resulting matter dominance in the universe are observational evidence for a substructure beneath the Standard Model. It also suggests the particle horizon is an appropriate focus for efforts to link gravity with quantum mechanics.

Conflicts of Interest

The authors declare no conflicts of interest.

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