Coincidence problem in an oscillating universe

We analyze an oscillating universe model in brane world cenario. The oscillating universe cycles through a series of expansions and contractions and its energy density is dominated by dust matter at early-time expansion phase and by phantom dark energy at late-time expansion phase. We find that the period of the oscillating universe is not sensitive to the tension of the brane, but sensitive to the equation-of-state parameter w of the phantom dark energy, and the ratio of the period to the current Hubble age approximately varies from 3 to 9 when the parameter w changes from −1.4 to −1.1. The fraction of time that the oscillating universe spends in the coincidence state is also comparable to the period of the oscillating universe. This result indicates that the coincidence problem can be significantly ameliorated in the oscillating universe without singularity.     

Problems of a perpetually oscillating universe

A model is constructed where a Friedmann universe, when collapsing, passes the region of Planek's dimensions near the classical singularity in the De Sitter state. The model assumes that the condition of the one-loop approximation $\text{R}{}_{\mathrm{\mu \nu \lambda \delta }}\text{· R}{}^{\mathrm{\mu \nu \lambda \delta }}\text{≤}\text{1}\text{l}{}_{\mathrm{<mtext>P1</mtext>}}{}^4$ is a universal law of nature. In the case of a dust-like matter the law restricts the mass density (?) to Planck's density $\text{?}{}_{\mathrm{<mtext>P1</mtext>}}\text{=}\text{c}{}^5\text{khx}{}^2$; $\text{?}{}^2\text{?}{}_{\mathrm{<mtext>P1</mtext>}}{}^2\text{≤ 1}$. In the dust-like model it is assumed that the gravitation constant χ depends on the density as $\text{χ = χ}{}_0\text{φ(}\text{?}{}^2\text{?}{}_{\mathrm{<mtext>P1</mtext>}}\text{?1)}$, the function φ vanishes at ? = ?_P1 so that the matter tensor in the right-hand side of the Einstein equation χT_μ^ν disappears in this limit, and the Friedmann universe becomes a De Sitter universe whose Λ¹ term is written in the form $\text{Λ}{}^1\text{θ(}\text{?}{}^2\text{?}{}_{\mathrm{<mtext>P1</mtext>}}{}^2\text{)}$ and at ? → ?_P1, θ → 1. As kh → 0, the theory becomes classical. Some difficulties of a perpetually oscillating model, namely, entropy increase, mass increase due to particle production, and increase of metric perturbations (appearance of gravitational waves) in the process of collapse, are considered in the framework of the model. Various possibilities of the mathematical apparatus of the theory that naturally involve limitations on the curvature value and, in particular, nonlinear Born-type lagrangians are discussed.     

Analogue of the Kapitza pendulum based on a compass arrow in an oscillating magnetic field

Magnetic analogues of the Kapitza pendulum have been implemented in systems formed by one or two compass arrows in an oscillating magnetic field. The complete state diagrams for the systems studied have been determined. It is experimentally confirmed that two dynamically stabilized equilibrium states coexist in the system of two magnetic arrows.     

Time-reversal symmetry violation and the oscillating universe

The expressions for the fractional number ofK ⁰'s and¯K ⁰'s in a neutral kaon beam are discussed with reference to time-reversal asymmetry. The suggested relation between the sign of Re ( is the Lee-WuT-violation parameter) and the cosmological arrow of time ifCPT is broken is further clarified.Research sponsored by the Air Force Office of Scientific Research, Office of Aerospace Research, U.S. Air Force, under AFOSR grant number EOOAR-68-0010, through the European Office of Aerospace Research.     

The arrow of time and the expansion of the universe

It is pointed out that a model used to test any suggestion regarding the arrow of time in a cosmological contect, must have sufficient complexity. The clain of Zeh that the arrow of time defined by a universal wavefunction does not permit a reversal of cosmic expansion to be observed, is refuted on these grounds.     

Asymptotic freedom and entropy in a perpetually oscillating universe

A model of a perpetually oscillating universe is considered. In this model the universe, when contracting to Planck dimensions, transforms from the Friedmann to the De Sitter phase with one and the same $\text{Λ ～}\text{1}\text{l}{}^2{}_{\mathrm{<mtext>P</mtext><mtext>1</mtext>}}$, irrespective of the value of the total bare mass of the Friedmann universe.     

Tachyons in an expanding universe

It has been suggested that causality problems associated with tachyons can be eliminated by the existence of a perferred frame of rest in which backward time travel is impossible. Furthermore, cosmology provides a de facto preferred rest frame. However, it is demonstrated here that the observed expansion of the universe raises further problems for the existence of tachyons.     

Electrodynamics in an expanding universe

An algebraic form of the energy momentum tensor of the electromagnetic field is derived in terms of two scalars and two mutually orthogonal vector fields. Upon inserting this tensor into the field equations, solutions of the co-determined Einstein-Maxwell equations are obtained. The line element used is that corresponding to a conformal flat universe, whose form is then uniquely determined by the field equations. The case of a charged fluid is also considered and it is found that the particular form of the velocity field chosen limits the choice of the possible equation of state connecting the pressure and density distributions.     

Two-state system in an oscillating field

We consider two states connected by two channels, one of which is activated but the other has no potential barrier. The height of the barrier is oscillating together with an external ac-field. We find that an external field shifts the average populations of the states and tends to equalize them. The steady-state flux circulates along the close circuit formed by these channels.     

Quantum mechanics in an entirely deterministic universe

It is argued that, according to the suggested interpretation of quantum mechanical probabilities, (1) the Bell inequalities are not equivalent with those inequalities derived by Pitowsky and others that indicate the Kolmogorovity of a probability model, (2) the original Bell inequalities are irrelevant to both the question of whether or not quantum mechanics is a Kolmogorovian theory as well as the problem of determinism, whereas (3) the Pitowsky-type inequalities are not violated by quantum mechanics, hence (4) quantum mechanics is a Kolmogorovian probability theory, therefore, (5) it is compatible with an entirely deterministic universe.On leave from the Institute for Theoretical Physics, Eötvös University, Budapest, Hungary.