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Showing papers on "Particle horizon published in 2017"


Journal ArticleDOI
H. Yu, Fa-Yin Wang1
TL;DR: In this paper, the authors derived the proper distance-redshift relation from dispersion measures (DMs) of repeat fast radio burst (FRB) with measured redshifts from Monte Carlo simulations.
Abstract: The cosmic proper distance $d_P$ is a fundamental distance in the Universe. Unlike the luminosity and angular diameter distances, which correspond to the angular size, the proper distance is the length of light path from the source to observer. However, the proper distance has not been measured before. The recent redshift measurement of a repeat fast radio burst (FRB) can shed light on the proper distance. We show that the proper distance-redshift relation can indeed be derived from dispersion measures (DMs) of FRBs with measured redshifts. From Monte Carlo simulations, we find that about 500 FRBs with DM and redshift measurements can tightly constrain the proper distance-redshift relation. We also show that the curvature of our Universe can be constrained with a model-independent method using this derived proper distance-redshift relation and the observed angular diameter distances. Owing to the high event rate of FRBs, hundreds of FRBs can be discovered in the future by upcoming instruments. The proper distance will play an important role in investigating the accelerating expansion and the geometry of the Universe.

55 citations


Journal ArticleDOI
TL;DR: In this paper, the authors quantify the notion of cosmic information (CosmIn) for an eternal observer in the universe, which requires the universe to have a late-time accelerated expansion.

32 citations


Journal ArticleDOI
TL;DR: In this article, the authors propose an interpretation of the expansion and acceleration of the universe from an information theoretic viewpoint and obtain the time evolution of the configuration entropy of the mass distribution in a static universe and show that the process of gravitational instability leads to a rapid dissipation of configuration entropy during the growth of the density fluctuations making such a universe entropically unfavourable.
Abstract: We propose an interpretation of the expansion and acceleration of the Universe from an information theoretic viewpoint We obtain the time evolution of the configuration entropy of the mass distribution in a static Universe and show that the process of gravitational instability leads to a rapid dissipation of configuration entropy during the growth of the density fluctuations making such a Universe entropically unfavourable We find that in an expanding Universe, the configuration entropy rate is governed by the expansion rate of the Universe and the growth rate of density fluctuations The configuration entropy rate becomes smaller but still remains negative in a matter dominated Universe and eventually becomes zero at some future time in a $\Lambda$ dominated Universe The configuration entropy may have a connection to the dark energy and possibly plays a driving role in the current accelerating expansion of the Universe leading the Universe to its maximum entropy configuration

30 citations


Journal ArticleDOI
TL;DR: In this article, the authors studied wormholes solutions based on fractional action cosmology and derived wormholes wave function in a closed Friedmann-Robertson-Walker (FRW) universe and found that a wormhole can survive in the presence of quantum effects only if the expansion of the universe is accelerated with time.
Abstract: In this work we study wormholes solutions based on fractional action cosmology. We discuss cosmic dynamics of the universe in the presence of wormhole and wormhole wave function in closed Friedmann–Robertson–Walker (FRW) universe. We have observed that cosmic acceleration with traversable wormhole may be realized without the need of exotic matter like dark and phantom energy unless the scale factor of the universe obeys a power law dominated by a negative fractional parameter, which is constrained from type Ia supernovae data. Besides, we have derived wormholes wave function in a closed FRW universe and we have found that a wormhole can survive in the presence of quantum effects only if the expansion of the universe is accelerated with time.

25 citations


Journal ArticleDOI
TL;DR: In this article, the existence and stability of the Einstein static universe under the generalized uncertainty principle (GUP) effects was studied. And the authors showed that the scale factor of the universe for closed deformed isotropic and homogeneous FLRW universe depends on the GUP coupling parameter α.

23 citations


Journal ArticleDOI
TL;DR: In this paper, a simple method for the description of the big bang was proposed for the flat Friedmann universe, which gives the same results as more complicated methods, using Weyl symmetry or the transitions between the Jordan and Einstein frames.
Abstract: We consider a rather simple method for the description of the big bang--big crunch cosmological singularity crossing. For the flat Friedmann universe this method gives the same results as more complicated methods, using Weyl symmetry or the transitions between the Jordan and Einstein frames. It is then easily generalized for the case of a Bianchi-I anisotropic universe. We also present early-time and late-time asymptotic solutions for a Bianchi-I universe, filled with a conformally coupled massless scalar field.

22 citations


Journal ArticleDOI
TL;DR: In this article, the CMB quadrupole constraint on the amplitude of the initial fluctuations and the size of the observable universe relative to a length scale characterizing the ultra-large scale structure (ULSS) was investigated.
Abstract: Cosmic inflation, a period of accelerated expansion in the early universe, can give rise to large amplitude ultra-large scale inhomogeneities on distance scales comparable to or larger than the observable universe. The cosmic microwave background (CMB) anisotropy on the largest angular scales is sensitive to such inhomogeneities and can be used to constrain the presence of ultra-large scale structure (ULSS). We numerically evolve nonlinear inhomogeneities present at the beginning of inflation in full General Relativity to assess the CMB quadrupole constraint on the amplitude of the initial fluctuations and the size of the observable universe relative to a length scale characterizing the ULSS. To obtain a statistically meaningful ensemble of simulations, we adopt a toy model in which inhomogeneities are injected along a preferred direction. We compute the likelihood function for the CMB quadrupole including both ULSS and the standard quantum fluctuations produced during inflation. We compute the posterior given the observed CMB quadrupole, finding that when including gravitational nonlinearities, ULSS curvature perturbations of order unity are allowed by the data, even on length scales not too much larger than the size of the observable universe. Our results illustrate the utility and importance of numerical relativity for constraining early universe cosmology.

21 citations


Journal ArticleDOI
TL;DR: In this article, the authors investigated the anisotropic behavior of the accelerating universe in Bianchi V spacetime in the framework of General Relativity (GR), where the matter field is of two non-interacting fluids, i.e. the usual string fluid and dark energy (DE) fluid.
Abstract: In this paper, we have investigated the anisotropic behavior of the accelerating universe in Bianchi V spacetime in the framework of General Relativity (GR). The matter field we have considered is of two non-interacting fluids, i.e. the usual string fluid and dark energy (DE) fluid. In order to represent the pressure anisotropy, the skewness parameters are introduced along three different spatial directions. To achieve a physically realistic solutions to the field equations, we have considered a scale factor, known as hybrid scale factor, which is generated by a time-varying deceleration parameter. This simulates a cosmic transition from early deceleration to late time acceleration. It is observed that the string fluid dominates the universe at early deceleration phase but does not affect nature of cosmic dynamics substantially at late phase, whereas the DE fluid dominates the universe in present time, which is in accordance with the observations results. Hence, we analyzed here the role of two fluids in ...

21 citations


Posted Content
TL;DR: In this paper, the authors tackle the vast question of generating accelerated periods of expansion of the universe and propose a model based on the idea of an accelerated expanding universe being a mirage due to inhomogeneities disposed in a fractal way.
Abstract: This thesis tackles the vast question of generating accelerated periods of expansion of the universe. Models loosely related were developed in the early and late universe. In the early universe, generalizations of the Schwinger effect were developed in curved (de Sitter) space and some backreaction effects were estimated. In the late universe, a fractal model was developed and confronted to supernovae data. This relies on the idea of an accelerated expanding universe being nothing but a mirage due to inhomogeneities disposed in a fractal (in this particular model) way. Finally a model of interacting energy based on an Einstein-Cartan gravitational theory was phenomenologically investigated.

16 citations


Journal ArticleDOI
A. I. Keskin1
TL;DR: In this article, the authors presented a super inflation mechanism composed of three phase regions which describes the evolution of the early universe and verified this inflationary mechanism by using the spectral index parameter and the scalar tensor ratio.
Abstract: There are various mechanisms that explain both the inflationary epoch of the early universe and a unification of this epoch with the other stages of the universe. In this study, we show all the expansion history of the universe and transition among of them in a single form by using the theoretical framework of $F ( T, T_{G} ) $ gravity in the context of the FRW (Friedmann-Robertson-Walker) universe. According to a particular model we obtain the unified solutions of the field equations. Without using any scalar field description we especially present the super inflation mechanism composed of three phase regions which describes the evolution of the early universe. The mechanism begins with a vacuum state and then follows a super accelerated period where there are two regions. The first continues in a quintessential field, and the second is a region where the radiation is created. Furthermore, we verified this inflationary mechanism by using the spectral index parameter and the scalar tensor ratio, i.e., $n_{s}$ , $r$ , and calculated the ratio of radiation emergent from the quintessence field. This creation should be in a certain rate in the early universe otherwise we show that the universe cannot survive and continue to expand. Also, we have obtained a phantom solution of the model that shows two regions which are compatible with the recent cosmological observations. In one respect, it is observed that the late time expansion of the universe is similar to the early time inflation.

15 citations


Journal ArticleDOI
TL;DR: In this article, two consecutive Universes with positive cosmological constants filled with perfect fluids and conformal to the positive-spatial-curvature FLRW metric by an analytic conformal transformation have the following features implied by the Einstein equations.
Abstract: We show that two consecutive Universes with positive cosmological constants filled with perfect fluids and conformal to the positive-spatial-curvature FLRW metric by an analytic conformal transformation have the following features implied by the Einstein equations: a) the fluids can only belong to 4 classes (radiation, dust and two other classes with negative pressures corresponding to a gas of strings and a gas of domain walls), b) the field equations on both sides of the future/eternity hypersurface exhibit certain duality with the Einstein Universe at the background, and c) both eons (one at the end, and the other at the beginning) are almost critical, so that the future eon is dominated by radiation and resembles the beginning of our Universe.

Journal ArticleDOI
TL;DR: In this paper, a model of nonlinear electrodynamics with a dimensional parameter $\beta$ is considered and it is demonstrated that after the universe inflation the universe decelerates approaching the Minkowski spacetime.
Abstract: A model of nonlinear electrodynamics with a dimensional parameter $\beta$ is considered. Electromagnetic fields are the source of the gravitation field and inflation of the universe. We imply that the universe is filled by stochastic magnetic fields. It is demonstrated that after the universe inflation the universe decelerates approaching the Minkowski spacetime. We evaluate the spectral index, the tensor-to-scalar ratio, and the running of the spectral index which approximately agree with the PLANK and WMAP data.

Journal ArticleDOI
01 Jan 2017
TL;DR: In this paper, the authors hypothesize a closed universe belonging to the oscillatory class, where all the points are replaced by straight line segments: what we perceive as being a point is actually a straight line segment crossing the center of a four-dimensional ball.
Abstract: We hypothesize a closed Universe belonging to the oscillatory class. More precisely, we postulate a Universe that evolves following a simple harmonic motion whose pulsation is equal to the ratio between the speed of light and the mean radius of curvature. The existence of at least a further spatial dimension is contemplated. Although the space we are allowed to perceive is curved, since it is identifiable with a hypersphere whose radius depends on our state of motion, the Universe in its entirety, herein assimilated to a four-dimensional ball, is to be considered as being flat. All the points are replaced by straight line segments: In other terms, what we perceive as being a point is actually a straight line segment crossing the center of the above mentioned four-dimensional ball. In the light of these hypotheses, we can easily obtain the identity that represents the so called relativistic energy. In this paper we discuss, more thoroughly than elsewhere, the deduction of the so called mass-energy equivalence. Moreover, by carrying out a simple comparison with the way in which we perceive a bi-dimensional surface, the noteworthy concept of dimensional thickness is introduced.

Posted Content
01 Jan 2017-viXra
TL;DR: In this article, a new cosmological model is proposed for the dynamics of the universe and the formation and evolution of galaxies and it is shown that the matter of the Universe contracts and expands in cycles, and that galaxies in a particular cycle may have imprints from the previous cycle.
Abstract: A new cosmological model is proposed for the dynamics of the Universe and the formation and evolution of galaxies. It is shown that the matter of the Universe contracts and expands in cycles, and that galaxies in a particular cycle may have imprints from the previous cycle. It is proposed that RHIC’s liquid gets trapped in the cores of galaxies in the beginning of each cycle and is liberated throughout time and is, thus, the power engine of AGNs. It is also proposed that the large-scale structure is a permanent property of the Universe, and thus, it is not created. It is proposed that spiral galaxies and elliptical galaxies are formed by mergers of nucleon vortices (vorteons) at the time of the big squeeze and immediately afterwards and that the merging process, in general, lasts an extremely long time, of many billion years. The origin of quasars is explained and the evaporation rate of RHIC’s liquid is calculated. The large mass at the center of quasar PDS 456 is calculated and agrees in order of magnitude with that attributed to a supposed black hole. It is concluded that the Universe is eternal and that space should be infinite or almost.

Journal ArticleDOI
TL;DR: In this article, a topological defect created by spontaneous breaking of the U(1) symmetry prior to inflation generated an initial phase variation across the observable region of the universe, and the amplitude of this phase fluctuation is protected by topology if the defect is inside the horizon, and is frozen by causality if it exits the horizon.
Abstract: Observations indicate that large-scale anomalies exist in the fluctuations of the cosmic microwave background. In these anomalies, the hemispherical power amplitude asymmetry has a correlation length comparable to that of the observable universe. We propose that a topological defect created by spontaneous breaking of the U(1) symmetry prior to inflation generated an initial phase variation, $\ensuremath{\delta}\ensuremath{\theta}$, across the observable region of the universe. The amplitude of this phase fluctuation is protected by topology if the defect is inside the horizon, and is frozen by causality if the defect exits the horizon. After inflation, the phase-corresponding boson field started to oscillate, when the Hubble rate decreased to a level comparable to the mass of the boson field. The energy density of the newly created boson particles varied across the observable universe. The bosons subsequently decayed into radiation prior to the big bang nucleosynthesis epoch, and the resulting fluctuations in the energy density produced the observed power asymmetry. This scenario predicts a scale-dependent modulation amplitude power asymmetry and in addition, as topological defects created by phase transitions are a very general phenomenon, the observed hemispherical asymmetry may be seen as an evidence for the cosmological inflation.

Journal ArticleDOI
10 Mar 2017-Science
TL;DR: Debate over the Hubble constant, the expansion rate of the universe, has exploded again, and the dispute suggests a missing ingredient may be fueling the growth of the universes.
Abstract: Debate over the Hubble constant, the expansion rate of the universe, has exploded again. Astronomers had mostly settled on a number using a classical technique—the "distance ladder," or astronomical observations from the local universe on out. But these values conflict with cosmological estimates made from maps of the early universe and adjusted to the present day. The dispute suggests a missing ingredient may be fueling the growth of the universe.

Journal ArticleDOI
TL;DR: In this article, it is shown that in the early Universe the orientation of its spin is random, and the cosmological principle is satisfied, and this result is naturally consistent with the CMBisotropy.
Abstract: We find the probability density distribution of torque orientations in the Universe for the entire period of its evolution. It is shown that in the early Universe the orientation of its spin is random, and the cosmological principle is satisfied. This result is naturally consistent with the CMBisotropy. In the modern Universe the rotation axis direction becomes anisotropic, and the cosmological principle, strictly speaking, is not satisfied. This is confirmed by the large-scale anisotropy in the distribution of space objects and by the torque alignment direction. But since the value of the angular velocity of our Universe is $$\omega_{U_{n}}\sim10^{-19}\;\text{Hz}$$ , finding of such rotation and its influence on the natural processes is extremely difficult. So today dominates the view that the Universe is isotropic, and the cosmological principle is satisfied in it.

Journal ArticleDOI
TL;DR: In this article, the authors investigated the stability of the universe under linear scalar, vector, and tensor perturbations in the context of a deformed Hoˇrava-Lifshitz cosmology related to entropic forces.
Abstract: We investigate the stability of the Einstein static universe under linear scalar, vector, and tensor perturbations in the context of a deformed Hoˇrava-Lifshitz (HL) cosmology related to entropic forces. We obtain a general stability condition under linear scalar perturbations. Using this general condition, we show that there is no stable Einstein static universe in the case of a flat universe (k = 0). In the special case of large values of the parameter ω of HL gravity in a positively curved universe (k > 0), the domination of the quintessence and phantom matter fields with a barotropic equation of state parameter β −1/3 must be the dominant fields of the universe. We also demonstrate a neutral stability under vector perturbations. We obtain an inequality including the cosmological parameters of the Einstein static universe for stability under tensor perturbations. It turns out that for large values of ω, there is stability under tensor perturbations.

Journal ArticleDOI
TL;DR: In this article, the authors derived the distance within which two particles must be localized to give a black hole, which depends on the expansion rate of the background space, and then used this distance to calculate the number density, energy density and production rate of black holes produced in collisions of particles.
Abstract: According to a variant of the hoop conjecture, if we localize two particles within the Schwarzschild radius corresponding to their center of mass energy, then a black hole will form. Despite a large body of work on the formation of primordial black holes, so far this conjecture has not been generalized to expanding spacetimes. We derive a formula which gives the distance within which two particles must be localized to give a black hole, and which crucially depends on the expansion rate of the background space. In the limit of a very slow expansion, we recover the flat spacetime case. In the opposite limit of the large expansion rate when the inverse Hubble radius is smaller than the Schwarzschild radius of a "would be" black hole, the new critical distance between two particles that can make a black hole becomes equal to the particle horizon, which is just a requirement that the particles are in a causal contact. This behavior also nicely illustrates why the Big Bang singularity is not a black hole. We then use our formula to calculate the number density, energy density and production rate of black holes produced in collisions of particles. We find that though black holes might be numerous at high temperatures, they never dominate over the background radiation below the Planck temperature.

Journal ArticleDOI
TL;DR: In this paper, it is shown that some time after the matter in the universe is diluted enough, at, the decelerating expansion shifts spontaneously to an accelerating one without a dark energy.
Abstract: Lorentz gauge theory of gravity was recently introduced. We study the homogeneous and isotropic universe of this theory. It is shown that some time after the matter in the universe is diluted enough, at , the decelerating expansion shifts spontaneously to an accelerating one without a dark energy. We discuss that Lorentz gauge theory puts no constraint on the total energy content of the universe at present time and therefore the magnitude of vacuum energy predicted by field theory is not contradictory anymore. It is demonstrated that in this theory the limit on the number of relativistic particles in the universe is much looser than in GR. An inflationary mechanism is discussed as well. We show that the theory, unlike GR, does not require the slow-roll or similar conditions to drive the inflation at the beginning of the universe.

Journal ArticleDOI
TL;DR: In this paper, the authors address the issue related to the particle horizon problem in the bouncing universe models and present a toy example of a bouncing universe where they specify the conditions which dictate the presence of a particle horizon.
Abstract: As our understanding of the past in a bouncing universe is limited, it becomes difficult to propose a cosmological model which can give some understanding of the causal structure of the bouncing universe. In this article we address the issue related to the particle horizon problem in the bouncing universe models. It is shown that in many models the particle horizon does not exist, and consequently the horizon problem is trivially solved. In some cases a bouncing universe can have a particle horizon and we specify the conditions for its existence. In the absence of a particle horizon the Hubble surface specifies the causal structure of a bouncing universe. We specify the complex relationship between the Hubble surface and the particle horizon when the particle horizon exists. The article also address the issue related to the event horizon in a bouncing universe. A toy example of a bouncing universe is first presented where we specify the conditions which dictate the presence of a particle horizon. Next we specify the causal structures of three widely used bouncing models. The first case is related to quintom matter bounce model, the second one is loop quantum cosmology based bounce model and lastly $f(R)$ gravity induced bounce model. We present a brief discussion on the horizon problem in bouncing cosmologies. We point out that the causal structure of the various bounce models fit our general theoretical predictions.

Posted Content
TL;DR: In this paper, it was shown that the capacity of the universe to measure time must be at least as large as the number of clock "ticks" that need to be recorded somewhere within the universe.
Abstract: Modern physics has unlocked a number of mysteries regarding the early Universe, such as the baryogenesis, the unification of the strong and electroweak forces and the nucleosynthesis. However, understanding the very early Universe, close to the Planck epoch, still presents a major challenge. The theory of inflation, which is assumed to have taken place towards the end of the very early Universe, has been introduced in order to solve a number of cosmological problems. However, concrete observational evidence for inflation is still outstanding and the physical mechanisms behind inflation remain mostly unknown. In this paper we argue for inflation from a different standpoint. In order for time to have any concrete physical meaning in the very early and the early Universe, the capacity of the Universe to measure time - its size or, equivalently, memory - must be at least as large as the number of clock "ticks" that need to be recorded somewhere within the Universe. Using this simple criterion, we provide a sketch proof showing that in the absence of inflation the subsystems of the Universe might not have been able to undertake the synchronised evolution described by the time we use today.

Posted Content
TL;DR: In this article, it is shown that the interaction of the electromagnetic field with the vacuum of the electron-positron field gives rise to dependence of the speed of light propagation on the radiation temperature.
Abstract: It is shown that the interaction of the electromagnetic field with the vacuum of the electron-positron field gives rise to dependence of the speed of light propagation on the radiation temperature. Estimation show that in the modern epoch, even at very high temperatures, such for example which exist in the star interiors, the temperature-dependent correction to the speed of light proves to be extremtly small. But in the cosmological model of the hot Universe, in the first instances after the Big Bang the temperature was so high that the speed of light exceeded its present value by many orders of magnitude. The effect of dependence of the speed of light on temperature must be important for understanding the early evolution of the Universe.

Posted Content
01 Jul 2017-viXra
TL;DR: The cosmological constant of quantum mechanics is closely related to Planck's constant of the universe, save for its time dependence as mentioned in this paper, and the time dependence depends on the number of atoms in the universe.
Abstract: (H-Z) x mc^2 "quanta of the universe", universe matter density and the cosmological constant are all closely related to Planck's constant of quantum mechanics save for its time dependence.

Journal ArticleDOI
29 Apr 2017-Universe
TL;DR: In this article, the concept of causal mass is defined in a cosmological context, and discussed in relation to the cosmic inertial dragging effect, and the mass inside the particle horizon of the flat ΛCDM-model integrated along the past light cone is calculated.
Abstract: In order to provide a better understanding of rotating universe models, and in particular the Godel universe, we discuss the relationship between cosmic rotation and perfect inertial dragging. In this connection, the concept of causal mass is defined in a cosmological context, and discussed in relation to the cosmic inertial dragging effect. Then, we calculate the mass inside the particle horizon of the flat ΛCDM-model integrated along the past light cone. The calculation shows that the Schwarzschild radius of this mass is around three times the radius of the particle horizon. This indicates that there is close to perfect inertial dragging in our universe. Hence, the calculation provides an explanation for the observation that the swinging plane of a Foucault pendulum follows the stars.

Posted ContentDOI
TL;DR: In this article, a simple toy model corresponding to a network of frustrated topological defects of domain walls or cosmic strings that exist previous to the standard slow-roll inflationary era of the universe is presented.
Abstract: There is an apparent power deficit relative to the Lambda-CDM prediction of the CMB spectrum at large scales, which, though not yet statistically significant, persists from WMAP to Planck data. We first present a simple toy model corresponding to a network of frustrated topological defects of domain walls or cosmic strings that exist previous to the standard slow-roll inflationary era of the universe. Those features are phenomenologically modeled by a Chaplygin gas that can interpolate between a network of frustrated topological defects and a de Sitter-like or a power-law inflationary era. We show that these scenarios can alleviate the quadrupole anomaly of the CMB spectrum, based on the approximate initial conditions for the long-wavelength perturbations. We then go further to show that the large-scale spectrum at the end of inflation reflects the super-horizon spectrum of the initial state of the inflaton field. By studying the curvature perturbations of a scalar field in the FLRW universe parameterized by the equation of state parameter w, we find that the large-scale spectrum is suppressed if the universe begins with the adiabatic vacuum in a superinflation (w 0) era. In the latter case, there is however no causal mechanism to establish the initial adiabatic vacuum. To search for a more realistic initial condition of the inflationary universe, we consider the Hartle-Hawking no-boundary wave function, which is a solution to the Wheeler-DeWitt equation, as the initial condition of the universe. We find that the power suppression can be the consequence of a massive inflaton, whose initial vacuum is the Euclidean instanton in a compact manifold. We calculate the primordial power spectrum of the perturbations and show that, as long as the scalar field is moderately massive, the power spectrum is suppressed at the long-wavelength scales.

01 Jan 2017
TL;DR: In this article, the authors considered properties of Scalar Field, which is responsible for the creation of matter in all layers of the fiberspace of the super-Universe, and showed that the Field generates all known fields in the universe.
Abstract: Starting from earlier developed by author model of origin of the Universe with minimal initial entropy, in this paper we consider properties of Scalar Field, which is responsible for the creation of matter in all layers of the fiberspace of Super-Universe. It allows to explain all the known processes occurring in the Microcosm and the Macrocosm of our Universe. It is shown that the Field generates all known fields in the Universe. The presence of the mass of elementary particles is provided by an influence of the Field, acting constantly in the Universe. The Field is characterized by high degree of symmetry in a multidimensional space, as well as two states with positive and negative energy. The integrity of the Universe provides an instant transfer of information and mutual “affection” of the particles within the total Universe, which is provided by the properties of the fiberspace and the Field.The latter sets a discreteness of time in our Universe time (time quant Δto = 7.36·10 s). The interaction of between particle and the corresponding antiparticle through the Field leads to the formation of Vacuum Particle. A World of Field-time is an inexhaustible source of energy that can be used by mankind.

Posted Content
TL;DR: In this article, the authors studied how a minimal generalization of Einstein's equations might generate a dynamical mechanism to explain the special initial condition necessary to obtain the homogeneous and flat universe we observe today.
Abstract: We study how a minimal generalization of Einstein's equations, where the speed of light ($c$), gravitational constant ($G$) and the cosmological constant ($\Lambda$) are allowed to vary, might generate a dynamical mechanism to explain the special initial condition necessary to obtain the homogeneous and flat universe we observe today. Our construction preserves general covariance of the theory, which yields a general dynamical constraint in $c$, $G$ and $\Lambda$. We re-write the conditions necessary in order to solve the horizon and flatness problems in this framework. This is given by the shrinking of the comoving particle horizon of this theory which leads to $\omega < -1/3$, but not necessarily to accelerated expansion like in inflation, allowing also a decelerated expansion, contraction and a phase transition in $c$, in the case of null $\Lambda$. We are able to construct the action of this theory, that describes the dynamics of a scalar field that represents $c$ or $G$ (and $\Lambda$). This action is general and can be applied to describe different cosmological solutions. We present here how the dynamics of the field can be used to solve the problems of the early universe cosmology by means of different ways to c-inflate the horizon in the early universe, solving the old puzzles of the cosmological standard model. Without a cosmological constant, we show that we can describe the dynamics of the scalar field representing $c$ given a potential, and derive the slow-roll conditions that this potential should obey. In this setup we do not have to introduce an extra unknown scalar field, since the degree of freedom associated to the varying constants plays this role, naturally being the field that is going to be responsible for inflating the horizon in the early universe.


Journal ArticleDOI
09 Jun 2017
TL;DR: In this article, a cosmology with a non-zero Λ vacuum energy is presented, where the initial radius of the universe is set in four dimensions and if there is only one repeating universe, then the initial radii of a universe is R → 0 or gets very close to zero if we use the Einstein Equations modified by Stoica.
Abstract: When the initial radius of the universe is set in four dimensions and if there is only ONE repeating universe, then the initial radii of the universe is R → 0 or gets very close to zero if we use the Einstein Equations modified by Stoica. The Einstein Equations are reset by Stoical in a formalism which removes in four dimensions, the big bang singularity pathology. So then the reason for Planck length no longer holds. This manuscript assumes a repeating single universe. We present entanglement entropy in the early universe with a shrinking scale factor, due to Muller and Lousto, and show that there are consequences due to initial entangled for a time dependent horizon radius in cosmology, with (flat space conditions) for conformal time. Even if the 3-dimensional spatial length goes to zero. Our new manuscript presentation sets as a starting point a cosmology with a non-zero Λ vacuum energy. The non-zero Λ vacuum energy, initial configuration of the universe permits us to keep in an information theory stand point (information theory), computational bits for our configuration of cosmological expansion. This assemblage of computational bits occurs in cosmological evolution even if in an initial four-dimensional cosmology, we have the initial radii of the universe R → 0. We also find that in the case of a multiverse, such considerations will not hold and that cosmic singularities have a more different characteristic in the multiverse setting than in the single universe repeated over and over again, i.e. using an argument borrowed and modified from Kauffman, the multiverse will not mandate “perfect” singularities. The existence of a multiverse may allow for non zero singularities in lieu with the Kauffman argument cited at the end of the document, plus the lower pre big bang temperatures which may allow for the survival of gravitons just before the onset of the cosmological expansion phase, if a multiverse exists embedding our present universe.