Big Bang Universe Research Articles

Cosmic-ray neutrino annihilation on relic neutrinos revisited: a mechanism for generating air showers above the Greisen-Zatsepin-Kuzmin cutoff

If neutrinos are a significant contributor to the matter density of the universe, then they should have ∼ eV mass and cluster in galactic (super) cluster halos, and possibly in galactic halos as well. It was noted in the early 1980's that cosmic ray neutrinos with energy within δE E R = Γ Z M Z ∼ 3% of the peak energy E R = 4 (eV/ m ν ) × 10 21, eV will annihilate on the nonrelativistic relic antineutrinos (and vice versa) to produce the Z-boson with an enhanced, resonant cross section of O( G F ) ∼ 10 −32cm 2. The result of the resonant neutrino annihilation is a hadronic Z-burst 70% of the time, which contains, on average, thirty photons and 2.7 nucleons with energies near or above the GZK cutoff energy of 5 × 10 19 eV. These photons and nucleons produced within our Supergalactic halo may easily propagate to earth and initiate super-GZK air showers. Here we show that the probability for each neutrino flavor at its resonant energy to annihilate within the halo of our Supergalactic cluster is likely within an order of magnitude of 1%, with the exact value depending on unknown aspects of neutrino mixing and relic neutrino clustering. The absolute lower bound in a hot Big Bang universe for the probability to annihilate within a 50 Mpc radius (roughly a nucleon propagation distance) of earth is 0.036%. From fragmentation data for Z-decay, we estimate that the nucleons are more energetic than the photons by a factor ∼ 10. Several tests of the hypothesis are indicated.

The Origin of the Big Bang Universe in Ultimate Reality With Special Reference to the Cosmology of Stephen Hawking

En faisant reference a la cosmologie de Stephen Hawking, l'A. dessine les grandes lignes d'une riposte theiste a la theorie cosmologique contemporaine. En montrant qu'un subunivers mathematique et logique doit etre la condition pour la possibilite du big-bang, il developpe des arguments traditionnels en faveur d'un createur personnel de l'univers. Hawking affirme qu'il existe quelque chose qui peut creer le big-bang. Le subunivers provient directement de la realite ultime. Il agit non seulement pour creer le big-bang, mais assure la continuite de sa fonction tout au long de la vie de l'univers

In Search of a Key to the Universal Emergence: Comments on K. Sharpe’s ‘The Origin of the Big Bang Universe in Ultimate Reality with Special Reference to the Cosmology of Stephen Hawking’

In Search of a Key to the Universal Emergence: Comments on K. Sharpe’s ‘The Origin of the Big Bang Universe in Ultimate Reality with Special Reference to the Cosmology of Stephen Hawking’

OBSERVATIONAL COSMOLOGY AND NUMERICAL RELATIVITY

Abstract This paper brings together the theory of observational cosmology and the null-cone characteristic initial value problem (CIVP) of numerical relativity. A computer code is constructed which calculates the past behaviour of the Universe from input data that is, in principle, measurable. For practical reasons the code is limited to the case of axisymmetry without rotation. The construction of the code brings to light an interesting general point about observational cosmology. In a big-bang universe it is impossible, even in principle, to determine the state of the universe at early times. For the Einstein-de Sitter model this limit is t 0/27, where t 0 means now.

Can the vacuum foam structure solve the flatness problem of a big bang universe?

It seems the vacuum foam structure of the very early universe, together with the traversable Lorentzian wormholes inherent in it, could provide a very large statistical entropy, which means that we may easily solve the flatness problem in a big bang universe without inflation.

Observations which contradict the hypothesis of a big bang universe

The Big Bang theory requires all matter and galaxies to have been created simultaneously 15 billion years ago. But many young galaxies have been observed which must have been created more recently. Moreover, these younger objects, although demonstrably nearby, have large redshifts which cannot be due to recession velocity in an expanding universe. The fundamental assumption in the Big Bang is that extragalactic redshifts are caused only by the velocity of recession. It is shown here how every observational test which can be made on galaxies, and even stars, contradicts the assumption. It is described how a more general and more correct solution of the Einstein general relativity equations yields a non-expanding, continuous creation universe of unlimited age and size.

Narlikar's “Creation” of the Big Bang Universe was a Mere Origination

In Grünbaum (1989, 374, 390), I objected to Narlikar's (1977, 136–137) designation“event of ‘creation’”for asupposed first cosmic instant t= 0, which he imports into the big bang cosmology of the general theory of relativity (GTR). Narlikar (1992, 361–362) does reject a theological construal of the “creation”. But, endeavoring to justify his secular creationism, he now points out that, in the GTR, the usual derivation of matter-energy conservation from Hilbert's stationary action principle cannot beextendedto include the putativefirstinstantt= 0. Narlikar reasons that this “breakdown” in the derivation of energy conservation att =0 qualifies the putative initial event as the “creation event”. I argue that this inference is multiply fallacious.

The shadows of creation: dark matter and the structure of the universe

The Big-Bang Universe the particle connection shadows of doubt origins of the elements the creation of matter the birth of galaxies the heavens at large a burst of inflation the shadow world seeds of collapse probing the cosmos.

Cosmological Signatures in High S:N Spectra

We review briefly the observational status of abundance determinations for those elements produced in the first seconds of a “standard” Big Bang Universe, showing that although [4He] and [D] appear not to be mutually compatible there is still room for reconciliation via astration of D, for values consistent with estimated [7Li]. New limits to production cross-sections for 7Li appear to limit Nv (the number of light neutrino types) to no more than 3. Non-standard models with fluctuations are briefly considered; they are attractive because they use Ω = 1 and may also yield early C, N, O in significant quantities. The true value of 7Li [10-9 or 10−10 w.r.t. H] is the critical test here. We show where spectra of improved S:N are needed to progress in constraining cosmological models.

A First Order Phase Transition from Inflationary to Big Bang Universe

A First Order Phase Transition from Inflationary to Big Bang Universe

The dynamics of dimensional reduction

Kaluza-Klein theories possess extra spacetime dimensions which today must be highly compact, but which may have been dynamically important in the very early universe. In the self consistent models of Candelas and Weinberg the universe has to tunnel from some higher dimensional spacetime such as de Sitter space to a lower dimensional state through the nucleation of a bubble. This bubble then decays into the standard hot big bang universe.

Quark-hadron and chiral transitions and their relation to the early universe

A review is made of the relation of the quark-hadron and chiral symmetry transitions and the big bang universe. Possible signatures at de-confinement are mentioned and related to cosmology. It is noted that to produce surviving perturbations at this epoch requires black hole production which in turn would require a first-order phase transition. The effect of a quark matter phase in neutron stars is also discussed and related to monopole flux limits through its role in cooling.

Nonconservation of baryons in cosmology—revisited

The concept of the steady-state universe discussed by Hoyle & Narlikar two decades ago is revived in the light of the present discussions of the phase transition in the early big-bang universe. It is shown that with suitable scaling the bubble universe solution bears a striking similarity to the inflationary scenarios being discussed today. The currently discussed idea of cosmic baldness was also anticipated in the C-field cosmology of the steady- state universe.

Periodicity in the distribution of quasar redshifts and density perturbation in the early universe

We made a power spectrum analysis on the quasar emission redshift distribution, and further confirmed the existence of periodicity in respect of the quantity x = F ( z, q o ) defined at (8). The existence of this periodicity does not mean that the quasar redshift is non-cosmological, for it can be interpreted as a remnant of density (acoustic) perturbations in the early big-bang universe. For this model, we made a number of tests. We found: 1) the ratio of periodic to non-periodic components falls as the sample size increases; 2) the periodicity should be more marked for quasars in one region of the sky than for all quasars, and 3) the Jeans wavelength before the recombination epoch determines the length of the period. Using this model we also found that qo > 0.5, lending further support to the conclusion reached by other means that the universe may be closed.

Some Comments on a Stability of the S2 S2-Type Space-Time

In terms of the Abbott-Deser energy method, the stability for a small perturbation of N ariai's 5, ® s,. type solution of the vacuum Einstein equations with non-vanishing cosmological constant is studied. It is shown that the space-time is stable for some perturbations which arise only inside its event horizon. Recently, an effective cosmological term (A­ term) has been considered by many author·s in relation to the phase transition in an early stage of the big-bang universe. The de Sitter space­ time is famous as an exact solution of the vacuum Einstein equations with a positive cosmological constant A:

Quantum gravity and the “flatness problem” of the standard big bang universe

It is shown that, if the universe originated through quantum conformal fluctuations from the empty Minkowski space, then it is most likely to be spatially flat.

P ARTICLE PHYSICS IN THE VERY EARLY UNIVERSE*

Events in the very early big bang universe in which elementary particle physics effects may have been dominant are discussed, with attention to the generation of a net baryon number by way of grand unification theory, and emphasis on the possible role of massive neutrinos in increasing current understanding of various cosmological properties and of the constraints placed on neutrino properties by cosmology. It is noted that when grand unification theories are used to describe very early universe interactions, an initially baryon-symmetrical universe can evolve a net baryon excess of 10 to the -9th to 10 to the -11th per photon, given reasonable parameters. If neutrinos have mass, the bulk of the mass of the universe may be in the form of leptons, implying that the form of matter most familiar to physical science may not be the dominant form of matter in the universe.

The Physics-Astronomy Frontier

Spacetime diagrams and the structure of matter are considered, and aspects of electrical interaction are investigated. Attention is given to radiation, quantum mechanics, spectrum lines, black bodies, stellar spectra, the H-R diagram, radio astronomy, millimeter-wave astronomy, interstellar grains and infrared astronomy, and X-ray astronomy. The strong and weak interactions are examined, taking into account atoms, nuclei, the evolution of stars, and the measurement of astronomical distances. A description of gravitational interaction is also presented. The laws of motion and gravitation are considered along with black holes, the significance of cosmology, Hubble's law, the expanding universe, the symmetries of the universe, Olbers' paradox, the big-bang universe, Mach's principle, the meaning of the expansion of the system of galaxies, the redshift-magnitude relation of Hubble and Humason, the early universe, and the geometry of special relativity.

On the formation of collapsed superdense nuclei in the universe

The possibility of the production of putative superdense nuclei (SDNs) in the universe is studied with the assumption that the SDNs can certainly be formed when nucleons are compressed over some critical density. Possible nuclear astrophysical processes for SDN production taking place in the early big-bang universe, in interstellar space and in ejection from neutron stars are investigated. It is found that the SDNs cannot be produced at all in a hot universe regardless of the properties of SDNs. The situation that would occur in a cold universe is also discussed. A finite amount of SDNs is found to be formed in interstellar space as the product of high-energy reactions between primary cosmic rays and interstellar matter. It also becomes clear that the astration of SDNs thus formed plays no essential role for the enhancement of the number of SDNs. On the other hand, the SDNs originating from neutron stars are estimated to have a cosmic abundance relative to Si as high as 8 × 10 −8−−5, which is, apparently, in contradiction with observations. Some implications of this are discussed.

Galaxy formation: the first million years

An overview is given of the non-equilibrium behaviour conceivable during the first million years of the Universe’s life. We describe various classical and quantum processes of this type which might constrain and fashion the irregularity spectrum on large cosmic scales. The likely fate of adiabatic, isothermal and vortical fluctuations is traced through the radiation dominated phase of a hot, big-bang Universe. Both the linear and nonlinear behaviour of these fluctuations is discussed and it is indicated how different preferred mass scales and irregularity spectra might be expected to arise in association with them . * Singularity is almost invariably a clue. The more featureless and commonplace a crime is, the more difficult . . .’ (Sherlock Holmes: The Boscombe Valley mystery , by Arthur Conan Doyle).