Nonlinear Born Infeld Research Articles

Dark energy and neutrino superfluids

We show that the neutrino mass, the dark matter and the dark energy can be explained in a unified framework, postulating a new invisible Born–Infeld field, which we name “non-linear dark photon”, undergoing a meV-scale dynamical transmutation and coupled to neutrinos. Dark energy genesis is dynamically explained as a byproduct of the dark photon condensation, inducing the bare massless neutrinos to acquire an effective mass around the meV scale. It is fascinating to contemplate the channel induced by the non-linear dark photon leading to the pairing of the non-relativistic neutrinos, hence generating a cosmological superfluid state. As a consequence, the appearance of a light neutrino composite boson is predicted, providing a good cold dark matter candidate. In particular, if our model is enriched by an extra global Lepton number U L ( 1 ) symmetry, then the neutrino pair can be identified with a composite Majoron field with intriguing phenomenological implications for the neutrinoless-double-beta-decay ( 0 ν β β ) . Our model carries interesting phenomenological implications since dark energy, dark matter and the neutrino mass are time-varying dynamical variables, as a consequence of the non-linear Born–Infeld interaction terms. Limits arising from PLANCK+SNe+BAO collaborations data are also discussed. Finally, our model allows for an inverse hierarchy of neutrino masses, with interesting implications for the JUNO experiment.

Conductivity of the one-dimensional holographic p -wave superconductors in the presence of nonlinear electrodynamics

We investigate analytically as well as numerically effects of nonlinear Born-Infeld (BI) electrodynamics on the properties of (1+1)-dimensional holographic $p$-wave superconductor in the context of gauge/gravity duality. We consider the case in which the gauge and vector fields backreact on the background geometry. We apply the Sturm-Liouville eigenvalue problem for the analytical approach as well as the shooting method for the numerical calculations. In both methods, we find out the relation between critical temperature $T_{c}$ and chemical potential $\mu$ and show that both approaches are in good agreement with each other. We find that if one strengthen the effect of backreaction as well as nonlinearity, the critical temperature decreases which means that the condensation is harder to form. We also explore the conductivity of the one-dimensional holographic $p$-wave superconductor for different values of b and $T/T_{c}$. We find out that the real and imaginary parts of the conductivity have different behaviors in higher dimensions. The effects of different values of temperature is more apparent for larger values of nonlinearity parameter. In addition, for the fixed value of $T/T_{c}$ by increasing the effect of nonlinearity we observe larger values for Drude-like peak in real part of conductivity and deeper minimum for imaginary part.

Finite-Energy Dressed String-Inspired Dirac-Like Monopoles

On extending the Standard Model (SM) Lagrangian, through a non-linear Born–Infeld (BI) hypercharge term with a parameter β (of dimensions of [mass] 2 ), a finite energy monopole solution was claimed by Arunasalam and Kobakhidze. We report on a new class of solutions within this framework that was missed in the earlier analysis. This new class was discovered on performing consistent analytic asymptotic analyses of the nonlinear differential equations describing the model; the shooting method used in numerical solutions to boundary value problems for ordinary differential equations is replaced in our approach by a method that uses diagonal Padé approximants. Our work uses the ansatz proposed by Cho and Maison to generate a static and spherically-symmetric monopole with finite energy and differs from that used in the solution of Arunasalam and Kobakhidze. Estimates of the total energy of the monopole are given, and detection prospects at colliders are briefly discussed.

Optical properties of Born–Infeld-dilaton-Lifshitz holographic superconductors

In this letter, we first study the Lifshitz-dilaton holographic superconductors with nonlinear Born–Infeld (BI) gauge field and obtain the critical temperature of the system for different values of Lifshitz dynamical exponent, z, and nonlinear parameter b. We find that for fixed value of b, the critical temperature decreases with increasing z. This indicates that the increase of anisotropy between space and time (encoded in Lifshitz exponent z) prevents the phase transition. Also, for fixed value of z, the critical temperature decrease with increasing b. Then, we investigate the optical properties of (2+1) and (3+1)-dimensional BI-Lifshitz holographic superconductors in the presence of dilaton field. We explore the refractive index of the system. This is an important study, since it discloses the effects of anisotropy between space and time as well as nonlinearity of electrodynamics model and dimension on strange metamaterial behavior of the holographic superconductor. For z=1 and (2+1)-dimensional holographic superconductor, we observe negative real part for permittivity Re[ϵ] as frequency ω decreases. Thus, in low frequency region our superconductor exhibit metamaterial property. This behavior is independent of the nonlinear parameter and can be seen for either linear (b=0) and nonlinear (b≠0) electrodynamics. Interestingly, for (3+1)-dimensional Lifshitz-dilaton holographic superconductors, we observe metamaterial behavior neither in the presence of linear nor nonlinear electrodynamics.

Black holes with constant topological Euler density

A class of four-dimensional spherically symmetric and static geometries with constant topological Euler density is studied. These geometries are shown to solve the coupled Einstein-Maxwell system when non-linear Born-Infeld–like electrodynamics is employed.

Extremal Einstein–Born–Infeld black holes in dilaton gravity

Motivated by considerable interests of Myers–Perry black holes, we employ the perturbative method to obtain a family of extremal charged rotating black hole solutions in odd dimensional Einstein–Born–Infeld-dilaton gravity. We start with an extremal Myers–Perry black hole with equal angular momenta, and then by adding the dilaton field and the nonlinear Born–Infeld electrodynamics, we find an extremal nonlinearly charged rotating black holes. The perturbative parameter is assumed to be the electric charge q and the perturbations are performed up to the third order. We then study the physical properties of these Born–Infeld-dilaton black holes. In particular, we show that the perturbative parameter, q, the dilaton coupling constant, α, and the Born–Infeld parameter, β, modify the Smarr formula and the values of the gyromagnetic ratio of the extremal charged rotating black holes.

On the NUT–Born–Infeld-[formula omitted] spacetime

The stationary axisymmetric spacetime coupled to nonlinear Born–Infeld electrodynamics is studied; the solution was derived by Plebański et al. (1984) in terms of integrals. It is characterized by six free parameters: mass, NUT charge, electric and magnetic charge, Born–Infeld parameter and cosmological constant. The geodesic and Lorentz force equations are integrated on the equatorial plane, and the effect of varying the parameters in the effective potential is analyzed. The trajectories of light and those for charged particles are discussed as well. Finally the conditions for the extreme black hole are determined, obtaining bounds between the charges, the Born–Infeld parameter and the cosmological constant.

Comparison Between the Nonlinear Born-Infeld and Coulomb Theories in Quantum Dots

Comparison Between the Nonlinear Born-Infeld and Coulomb Theories in Quantum Dots

Regular charged black hole construction in [formula omitted] dimensions

It is well known that unlike its chargeless version the charged Banados–Teitelboim–Zanelli (BTZ) black hole solution in (2+1)-dimensional spacetime is singular. We construct a charged, regular extension of the BTZ black hole solution by employing nonlinear Born–Infeld electrodynamics, supplemented with the Hoffmann term and gluing different spacetimes. The role of the latter term is to divide spacetime in a natural way into two regions by a circle and eliminate the inner singularity. Thermodynamics of such a black hole is investigated by Kaluza–Klein reduction to the (1+1)-dimensional dilaton gravity.

Cosmology with non-linear scalar field

Mukhanov and Vikman have studied inflation model with the non-linear (NL) scalar field. We discuss the dark energy model with the Lagrangian in the presence of the square potential. We analyse the sufficient condition for the existence of an attractor solution, and compare the equation of state parameter, the present age of universe and the transition redshift with the quintessence model. We also use the Gold dataset of 157 SN-Ia to finally constrain the parameter of the models. We find that the considered model is consistent with the observation and a little inferior to the quintessence model. The above Lagrangian is similar to the non-linear Born–Infeld (NLBI) scalar field model, while which is superior to the quintessence model.

A comparison of phantom linear scalar field and non-linear Born-Infeld scalar field

This paper studies phantom linear scalar field (LSF) and phantom non-linear Born-Infeld (NLBI) scalar field with square potential of the form V (ϕ) = \( \tfrac{1} {2} \)m2ϕ2. The equation of state parameter ω(z), and evolution of scale factor a(t) in both phantom LSF and phantom NLBI scalar model are explored. The age of universe H0t and the transition redshift Z are obtained. The Gold data set of 157-SN-Ia is used to constrain parameters of the two models by numerical calculation. The phantom LSF is slightly better than the phantom NLBI type scalar field model for a large m. Although a smaller m corresponding to a slower rolling of field \( \dot \varphi \) better fits the observation data, the difference between phantom NLBI scalar field and phantom LSF is not distinct in this case.

COSMOLOGY IN NONLINEAR BORN–INFELD SCALAR FIELD THEORY WITH NEGATIVE POTENTIALS

The cosmological evolution in Nonlinear Born–Infeld (hereafter NLBI) scalar field theory with negative potentials was investigated. The cosmological solutions in some important evolutive epoches were obtained. The different evolutional behaviors between NLBI and linear (canonical) scalar field theory have been presented. A notable characteristic is that NLBI scalar field behaves as ordinary matter nearly the singularity while the linear scalar field behaves as "stiff" matter. We find that in order to accommodate current observational accelerating expanding universe the value of potential parameters |m| and |V0| must have an upper bound. We compare different cosmological evolutions for different potential parameters m, V0.

A COMPARISON OF QUINTESSENCE AND NON-LINEAR BORN–INFELD SCALAR FIELD USING GOLD SUPERNOVA DATA

We study the Non-Linear Born–Infeld (NLBI) scalar field model and quintessence model with two different potentials (V(ϕ) = -sϕ and [Formula: see text]). We investigate the differences between these two models. We explore the equation of state parameter w and the evolution of scale factor a(t) in both the NLBI scalar field and quintessence model. The present age of universe and the transition redshift are also obtained. We use the Gold dataset of 157 SN-Ia to constrain the parameters of the two models. All the results show that the NLBI model is slightly superior to the quintessence model.

Dark Energy Model with Canonical Scalar Field and Non-Linear Born–Infeld Type Scalar Field

In this paper, we propose the non-linear Born–Infeld scalar field and canonical scalar field dark energy models with the potential \(\frac{\lambda }{4}( {\phi ^2 - \sigma ^2 })^2 + V_0\), which admits late time de Sitter attractor solution. The attractor solution corresponds to an equation of state ω_φ → − 1 and a cosmic density parameter Ω_φ → 1, which are important features for a dark energy model that can meet the current observations. dark energy; canonical scalar field, non-linear Born–Infeld type scalar field, attractor solution.

THE EVOLUTION OF THE UNIVERSE WITH THE B–I TYPE PHANTOM SCALAR FIELD

We consider the phantom cosmology with a Lagrangian [Formula: see text] originated from the nonlinear Born–Infeld type scalar field. This cosmological model can explain the accelerating expansion of the universe with the equation of state parameter w ≤ -1. We get a sufficient condition for an arbitrary potential that admits a late time attractor solution: the value of potential u(Xc) at the critical point (Xc, 0) should be maximum and greater than zero. We study a specific potential with the form of [Formula: see text] via phase plane analysis and compute the cosmological evolution by numerical analysis in detail. The results show that the phantom field survives till today (to account for the present observed accelerating expansion) without interfering with the nucleosynthesis of the standard model (the density parameter Ωϕ≃10-12 at the equipartition epoch), and also avoid the future collapse of the universe.

Remarks on the interaction between Born–Infeld solitons

We consider the abelian Higgs model as well as the SU(2) Georgi–Glashow model in which the gauge field action is replaced by a nonlinear Born–Infeld (BI) action. We study soliton solutions arising in these models, namely the vortex and monopole solutions, respectively. We construct formulae which provide good approximations for the mass of the BI deformed solitons using only the data of the undeformed solutions. The results obtained indicate that in the self-dual limit, the BI interaction leads to bound vortices, while for monopoles it gives rise to repulsion.