The signature of superstring balls near mini black holes at LHC

In this paper the information loss for fermionic superstrings “superstring balls” in mini black holes at LHC by extending the Gottesman and Preskill method to string theory and calculate the information transformation from the collapsing matter to the state of outgoing Hawking radiation is calculated. It is found that for all finite values of ω _n , all information from all string emission processes experiences some degree of loss. It means that the string model is not sufficient to solve the information-loss problem. Then the fermionic superstring states at corresponding point are considered. The correspondence principle offered a unique opportunity to test the Horowitz and Maldacena mechanism at correspondence point “the centre of mass energies around (M _s /(g _s )²)”. To consider the super string states, a copy of the original Hilbert space is constructed with a set of operators of creation/annihilation that have the same anticommutation properties as the original ones. The total Hilbert space is the tensor product of the two spaces H _physical ?H _unphysical , where in this case H _physical denotes the physical quantum states space of the fermionic string. It is shown that fermionic string states can be represented by a maximally entangled two-mode squeezed state of the physical and unphysical spaces of fermionic string. Also, the entropy for these string states is calculated. It is observed that black hole entropy matches the fermionic superstring entropy at transition point. This means that our result is consistent with correspondence principle and thus HM mechanism in string theory works. Finally the signature of fermionic string ball at LHC is studied. When superstring balls produce at LHC, they evaporate to Massive particles like Higgs boson. In fact string balls act as a factory for Higgs production. Then Higgs bosons decay to QCD matter. Thus an enhancement of QCD matter can be a signature of fermionic superstring ball at LHC.     

A new class of Inhomogeneous string cosmological models in general relativity

A new class of solutions of Einstein field equations has been investigated for inhomogeneous cylindrically symmetric space-time with string source. To get the deterministic solution, it has been assumed that the expansion (θ) in the model is proportional to the eigen value σ ¹  ₁ of the shear tensor σ ⁱ    _j . Certain physical and geometric properties of the models are also discussed.     

Entropy of viscous Universe models

The cosmological event horizon entropy and the apparent horizon entropy of the ΛCDM and the Bianchi type I Universe model with viscosity has been calculated numerically, and analytically in the large time limit. It is shown that for these Universe models the cosmological event horizon entropy increases with time and for large times it approaches a finite maximum value. The effect of viscosity upon the entropy is also studied and we have found that its role is to decrease the entropy. The bigger the viscosity coefficient is the less the entropy will be. Furthermore, the radiation entropy for the ΛCDM Universe model with and without viscosity is investigated, and together with the cosmological event horizon entropy are used to examine the validity of the generalized second law of thermodynamics, which states that the total rate of change of entropy of the Universe is never negative, in this Universe model.     

Inhomogeneous perfect fluid cosmologies in (4+1) dimensions

Exact solutions are obtained in (4+1) dimensions for plane symmetric and cylindrically symmetric inhomogeneous spacetimes. In the former case the three space depends on time only while the metric corresponding to the extra dimension is dependent on space as well as time coordinates. The cylindrically symmetric nonstatic solutions for the perfect fluid have no singularity near the axis, but show big bang type of singularity in the finite past. One of the classes of such solutions satisfies the barotropic equation of state of the form =p. Static solutions with cylindrically symmetric solutions are also obtained in 5 dimensions.     

Inhomogeneous cylindrically-symmetric models in string cosmology

In this paper, the Einstein field equations have been solved for inhomogeneous cylindrically symmetric space times with string source. Certain physical and geometrical properties of the models have been examined.     

Discrete source counts and the rotation of the local Universe in hierarchical cosmology

Attention is given to four reasons for believing that the upper limit on the rotation of the Universe ω set by isotropy of the 3K background may not be appropriate to the local system because of its hierarchical structure. In particular, recent work of Rubinet al. (1973) on the anisotropy of Hubble's parameter (H) as determined by certain galaxies is examined. The anisotropy inH is a 1st order harmonic effect, inconsistent with an origin in an acceleration of the expansion of the Universe (U _α;4≠0), but explicable as being due to a large peculiar velocity of the Local Group. This compromises limits set on ω by isotropy of the 3K field, as does the realization that only weak limits can be set if the last-scattering surface (z _*) is notz _*→∞ but is at smallz _* (as expected in a hierarchy). In a rotating Universe, the 3-spaces of constant density cannot be orthogonal on the world lines of matter: a number test of Gödell based on this is generalized and applied (after consideration of Galactic obscuration) to the local Universe, by taking data on clusters of galaxies from the Abell and Zwicky catalogues. Data from the former give only a marginally significant result for the component ω₁ of ω in one direction, but a bootstrap argument is applied which takes significance over from Abell's data (considered as a class of galaxies) to Zwicky's data (taken as a class of clusters), giving a statistically significant result on the hypothesis that clusters are the fundamental units of the Universe: it seems likely that ω₁r?(const)r^-n with 0?n?1 over the interval 500–1000 Mpc (H=60 km s^?1 Mpc^?1) with a total rotation of ω<2ω₁, and ω₁ = 1.2 (+0.25) x 10^-18 s^-1 evaluated on data out to 10³ Mpc. Strictly, the quoted value of the rotation only applies to a region of space that in some sense has an isotropic limit: if the actual hierarchy has a large density-dependence away from a local origin (i.e., large thinning factor), then the numerical value of the rotation is smaller than the quoted value but still finite and significant.     

Compactification and cosmic string phenomenology

A U(1) model of gravitational, Higgs and, gauge fields is analysed. Two phases of the system are considered. In the case with broken symmetry we have the Nielsen-Olesen configuration. In the symmetric phase we find a space-time metric S² × E₁². This appears in full analogy to the Freund-Rubin compactification due to an antisymmeric tensor field. The connection of these structures with cosmic string phenomenology is analysed.     

String Cosmology With Magnetic Field in Cylindrically Symmetric Space-Time

In this paper, the Einstein field equations have been solved for inhomogeneous cylindrically symmetric space with string source in the presence of magnetic field. Certain physical and geometrical properties of the models have been examined. Also, the string solutions in which magnetic field are absent are discussed. This revised version was published online in July 2006 with corrections to the Cover Date.     

Effectively massive photons within Abelian Higgs galaxies

We demonstrate that photons emitted by spiral galaxies become effectively massive, if the latter are treated as macroscopic Abelian Higgs topological solitons. The rest mass of a photon is shown to be proportional to the squared amplitude of the Higgs field distribution representing a ‘background’ static cylindrically symmetric magnetic vorto-source (-sink). Because the amplitude increases in a monotonous fashion from zero at the center of a spiral to a fixed non-zero value at its outer boundary, the rest mass (group velocity) of photons emitted at shorter distances from the galaxy' s center is smaller (greater) when compared to that of photons originating at larger distances. A rough estimate shows that for a spiral with a diameter of 60 kpc the maximum attainable mass of photon is of the order of 10⁻⁶⁰ g.     

The speed of light and the Hubble parameter: the Mass-Boom effect

We prove here that Newton’s universal gravitation and momentum conservation laws together reproduce Weinberg’s relation. It is shown that the Hubble parameter H must be built in this relation, or equivalently the age of the Universe t. Using a wave-to-particle interaction technique we then prove that the speed of light c decreases with cosmological time, and that c is proportional to the Hubble parameter H. We see the expansion of the Universe as a local effect due to the LAB value of the speed of light c ₀ taken as constant. We present a generalized red shift law and find a predicted acceleration for photons that agrees well with the result from Pioneer 10/11 anomalous acceleration. We finally present a cosmological model coherent with the above results that we call the Mass-Boom. It has a linear increase of mass m with time as a result of the speed of light c linear decrease with time, and the conservation of momentum mc. We obtain the baryonic mass parameter equal to the curvature parameter, Ω _m =Ω _k , so that the model is of the type of the Einstein static, closed, finite, spherical, unlimited, with zero cosmological constant. This model is the cosmological view as seen by photons, neutrinos, tachyons etc. in contrast with the local view, the LAB reference. Neither dark matter nor dark energy is required by this model. With an initial constant speed of light during a short time we get inflation (an exponential expansion). This converts, during the inflation time, the Planck’s fluctuation length of 10^?33 cm to the present size of the Universe (about 10²⁸ cm, constant from then on). Thereafter the Mass-Boom takes care to bring the initial values of the Universe (about 10¹⁵ gr) to the value at the present time of about 10⁵⁵ gr.     

The redshift-magnitude relation for galaxies

An analysis of the redshift-magnitude data for the 98 clusters of the list of Sandage and Hardy (1973) is repeated taking into account both the effect of richness and Bautz-Morgan classification on the absolute magnitude of the brightest members. We find that while the relationship between M and B-M class—whatever it is—does not change the value ofq ₀ theM-r relation is so dependent on the model of the Universe that we cannot use all the clusters in the analysis unless we establish that relation in an independent way. The analysis of richness 1 and 2 clusters support an open model of the Universe (q ₀<0.5) while the uncertainties in the attribution of richness to the three most distant clusters do not permit to discard the steady state.     

Delay of emission from extragalactic gamma-ray burst sources as a test for selecting a model of the universe

We obtained an order-of-magnitude estimate for the dispersion of light caused by the effect of quantum fluctuations on the propagation of electromagnetic waves in four-dimensional spacetime. We calculated the delay of the photons from cosmological gamma-ray bursts (GRBs) for the flat, open, and closed cosmological models. This delay is attributable to the effect of expansion of the Universe on the propagation of a dispersive light wave in space. Analysis shows that the delay of GRB photons contains a regular component related to the expansion of the Universe. We conclude that cosmological models of the Universe can be selected by the delay of emission of various energies from GRBs; the accuracy of measuring the parameter Δt/ΔE _γ must be no lower than 10^?6 s MeV^?1.     

Generalized Abelian Higgs sunspot endowed with a rotatory motion

An Abelian Higgs model of sunspot generalized in a Chern-Simons-like fashion is discussed. It is shown, in particular, that both themagnetic andelectric fields are present inside the sunspot, and that the latterrotates. One demonstrates that the total angular momentum of a static, cylindrically symmetric sunspot is proportional top ², wherep — an integer — stands for the number of magnetic fluxquanta carried by the spot. Finally, the behaviour of the Higgs field amplitude, magnetic and electric field strengths are illustrated for the spots carrying one to five flux quanta, all having the penumbra-to-umbra radius ratio of the value .     

Study of a new class of cylindrically symmetric space-time in general relativity

A new class of solutions of Einstein field equations is investigated for a cylindrically symmetric space-time when the source of gravitation is a perfect fluid. To get the deterministic solution a relation between metric coefficients A=(BC) ⁿ is assumed. Certain physical and geometric properties of the model are also discussed.     

Power-law and logarithmic entropy-corrected Ricci viscous dark energy and dynamics of scalar fields

In this work, I consider the logarithmic-corrected and the power-law corrected versions of the holographic dark energy (HDE) model in the non-flat FRW universe filled with a viscous Dark Energy (DE) interacting with Dark Matter (DM). I propose to replace the infra-red cut-off with the inverse of the Ricci scalar curvature R. I obtain the equation of state (EoS) parameter ω _Λ , the deceleration parameter q and the evolution of energy density parameter $\varOmega_{D}'$ in the presence of interaction between DE and DM for both corrections. I study the correspondence of the logarithmic entropy corrected Ricci Dark Dnergy (LECRDE) and power-law entropy corrected Ricci Dark Energy (PLECRDE) models with the the Modified Chaplygin Gas (MCG) and some scalar fields including tachyon, K-essence, dilaton and quintessence. I also make comparisons with previous results.     

Pilgrim dark energy in f(T,T G ) cosmology

We work on the reconstruction scenario of pilgrim dark energy (PDE) in f(T,T _G ). In PDE model it is assumed that a repulsive force that is accelerating the Universe is phantom type with (w _DE f(T,T _G ) models and correspondingly evaluate equation of state parameter for various choices of scale factor. Also, we assume polynomial form of f(T,T _G ) in terms of cosmic time and reconstruct H and w _DE in this manner. Through discussion, it is concluded that PDE shows aggressive phantom-like behavior for s=?2 in f(T,T _G ) gravity.     

Apparent superluminal velocities due to the curvature of space

Instead of the difficult concept of a three-dimensional curved space one can use two partial models of two-dimensional curved subspaces. If a two-dimensional subspace is curved the arbitrary angle of view must have a distorted shape which has in consequence an optical illusion. The distorted shape of ? must be corrected to the real angle¹φ, valid in uncurved space according to the relation φ=¹φf(ρ) where ρ is the central angle in theoretical sphere. If a two-dimensional subspace is just a spheric surface, the correction factor isf _s (ρ)?ρ/sin ρ, appropriate to the angle distance ρ from observer to the observed object. In this way it is possible to explain why, in remote parts of the Universe, it was observed that their assumed components were receding at velocities larger than that of light, because the correction factorf(ρ) can change up to infinity for ρ=π. On the other hand there are many clustering of galaxies, because the correction factor for a hyperbolic spool space or internal part of annuloid is between zero and one: 0<f _A (ρ))<1. Conception considered explains the cause of polarizing effect and interference phenomenon of light without assuming of components, too, but it is in contradiction with the recent interpretation of the spectrum. If we consider the Universe closed into itself due to curvature the existence of superluminal velocities is a undirect evidence for it. If we consider local hyperbolic spool spaces or that of annuloid, the existence of galaxies clustering is a needful but not sufficient condition for it.     

Observed characteristics of polar cleft Hα and OI emissions

Observations at Godhavn, Greenland show that the intersection of the polar cleft with the ionosphere can be recognized by simultaneous occurrence of hydrogen emissions (H_α, H_β>) and enhanced OI 6300 Å emission. The H_α-line reveals a characteristic narrow and symmetric Doppler profile which is interpreted as indicating that the solar wind protons retain their typical flux and energy spectrum all the way down to the ionosphere. The cleft intersection seems to cover the sector 04:00–22:00 geomagnetic time.