Narrow Results

In this paper we study neutral atoms of nuclear charge Z in a strong constant magnetic field of strength B. We improve the bound on confinement to the lowest Landau band given by Lieb, Solovej and Yngvason in [1]. This permits the calculation of the asymptotic form of the quantum current of atoms in the parameter region .

We compute general-relativistic polytropic models of magnetized rotating neutron stars, assuming that magnetic field and rotation can be treated as decoupled perturbations acting on the nondistorted configuration. Concerning the magnetic field, we develop and apply a numerical method for solving the relativistic Grad–Shafranov equation as a nonhomogeneous Sturm–Liouville problem with nonstandard boundary conditions. We present significant geometrical and physical characteristics of six models, four of which are models of maximum mass. We find negative ellipticities owing to a magnetic field with both toroidal and poloidal components; thus the corresponding configurations have prolate shape. We also compute models of magnetized rotating neutron stars with almost spherical shape due to the counterbalancing of the rotational effect (tending to yield oblate configurations) and the magnetic effect (tending in turn to derive prolate configurations). In this work such models are simply called "equalizers." We emphasize on numerical results related to magnetars, i.e. ultramagnetized neutron stars with relatively long rotation periods.

A synthesis of the present knowledge on gamma-ray emission from the magnetosphere of a rapidly rotating neutron star is presented, focusing on the electrodynamics of particle accelerators. The combined curvature, synchrotron, and inverse-Compton emission from ultra-relativistic positrons and electrons, which are created by two-photon and/or one-photon pair creation processes, or emitted from the neutron-star surface, provide us with essential information on the properties of the accelerator — electric potential drop along the magnetic field lines. A new accelerator model, which is a mixture of traditional inner gap and outer gap models, is also proposed, by solving the Poisson equation for the electrostatic potential together with the Boltzmann equations for particles and gamma-rays in the two-dimensional configuration and two-dimensional momentum spaces.

The possible mismatch between the theoretical and experimental absorption edge peaks in semiconductors in a magnetic field background may arise due to the approximation scheme used to analytically calculate the absorption coefficient. As a possible remedy we suggest to consider nontrivial boundary conditions on x–y plane by in-equivalently quantizing the exciton in background magnetic field. This inequivalent quantization is based on von Neumann's method of self-adjoint extension, which is characterized by a parameter Σ. We obtain bound state solution and scattering state solution, which in general depend upon the self-adjoint extension parameter Σ. The parameter Σ can be used to fine tune the optical absorption coefficient K(Σ) to match with the experiment.

The infrared sector of QCD contains all the necessary ingredients, once laid onto a time-dependent, curved background, to cater for the much needed cosmological vacuum energy. This is achieved through the fields that describe the impact of the long-range interactions of QCD, the Veneziano ghost and its dipolar partner. Although technically extremely challenging, the physics is well understood and the estimated dark energy density is of the correct order of magnitude. In this brief review I will retrace the steps leading to two new cosmological applications of this model, namely the possibility of the generation of cosmic magnetic fields, and the unification of several observed polarization anomalies under the same roof.

Recent observations of Stephan’s Quintet (SQ) gave new indications on its formation scenario. Older formation and role of NCG 7317 should be considered in revised numerical models of the compact group. Velocities of group members to recreate are estimated from redshift measurements. Several effects contribute to observed redshifts and a new effect is predicted to be the result of the gravitational interaction between photons and constant magnetic fields creating gravitational waves. The energy carried by these waves is manifested as redshifts of the photons. Cosmological simulation data are used to prove the significant contribution of our effect. The analysis of synthetic observations created from those simulations has shown that redshifts of SQ members could be misinterpreted as caused only from Doppler Effect. The revised models of the group should consider a new method to recreate the formation scenario based on redshift patterns and not mis-estimated velocities.

The origin of the cosmic rays at energies in excess of 10²⁰ eV is puzzling the scientific community for several decades now. The mystery adds to the general problem of understanding the nature of the bulk of cosmic rays, that are usually assumed to be accelerated within the Milky Way. Here we summarize the main elements of the observations and propose some possible avenues to interpret these data. The upcoming experiments for the detection of ultra high energy cosmic rays are expected to find the answers to many of our current open problems, and in particular to lead to the identification of the sources.

The excitation of cosmological perturbations in an anisotropic cosmological model and in the presence of a homogeneous magnetic field has been studied, using the ideal magnetohydrodynamic (MHD) equations. In this case, the system of partial differential equations which governs the evolution of the magnetized cosmological perturbations can be solved analytically. Our results verify that fast-magnetosonic modes propagating normal to the magnetic field, are excited. But, what is most important, is that, at late times, the magnetic-induction contrast(δB/B) grows, resulting in the enhancement of the ambient magnetic field. This process can be particularly favored by condensations, formed within the plasma fluid due to gravitational instabilities.

Gravitational instabilities in a magnetized Friedman–Robertson–Walker (FRW) universe, in which the magnetic field was assumed to be too weak to destroy the isotropy of the model, are known and have been studied in the past. Accordingly, it became evident that the external magnetic field disfavors the perturbations' growth, suppressing the corresponding rate by an amount proportional to its strength. However, the spatial isotropy of the FRW universe is not compatible with the presence of large-scale magnetic fields. Therefore, in this paper we use the general-relativistic version of the (linearized) perturbed magnetohydrodynamic equations with and without resistivity, to discuss a generalized Jeans criterion and the potential formation of density condensations within a class of homogeneous and anisotropically expanding, self-gravitating, magnetized fluids in curved space–time. We find that, for a wide variety of anisotropic cosmological models, gravitomagnetic instabilities can lead to subhorizontal, magnetized condensations. In the nonresistive case, the power spectrum of the unstable cosmological perturbations suggests that most of the power is concentrated on large scales (small k), very close to the horizon. On the other hand, in a resistive medium, the critical wave-numbers so obtained, exhibit a delicate dependence on resistivity, resulting in the reduction of the corresponding Jeans lengths to smaller scales (well bellow the horizon) than the nonresistive ones, while increasing the range of cosmological models which admit such an instability.

We obtain possibly valuable information about the phase diagram (tuned by the free orientation together with the Pauli blocking parameters) of rather dense matter at high fermion as well as boson number density but low temperature, which is not accessible to strong-magnetic-field experiments. The free orientation parameter we adopted could be due to the magnetic field or confined potentials. The possible coupling between the Pauli blocking and the induced (net) orientation (tuned by the strong magnetic field) is also addressed here which might be useful for the studies of very-strong magnetic fields in neutron stars.

We discuss the astronomical methods of searching for light Goldstone bosons (axions and arions). The basic idea is to use processes of coupling between axions and photons: a) the axion decay into two photons; b) the transformation process of photons into axions (arions) in the magnetic fields of stars and also of interstellar and intergalactic media; c) the inverse process of transformations of axions (arions) which are generated into cores of stars into X-ray photons. The decaying axions affect upon the diffuse extragalactic background radiation, the brightness of the night sky and especially on the intergalactic light of clusters of galaxies due to generation of the axion radiative decay emission line. The processes (b) and (c) are strongly dependent on polarization state of photon and may produce a noticeable amount of linear polarization.

The source of the universe inflation is electromagnetic fields obeying rational nonlinear electrodynamics proposed earlier. Within this model the singularities of the electric field at the center of charges, the Ricci scalar, the Ricci tensor squared and the Kretschmann scalar are absent. We consider the universe which is filled by stochastic magnetic fields. It is demonstrated that the inflation lasts approximately $2$ s with the reasonable $e$-folding number $N\approx 63$. The inflation starts from de Sitter space–time and after the universe inflation end it decelerates approaching the radiation era.

The aptitude of magneto-spectroscopic methods for studying the electronic and spin properties of semiconductor structures is demonstrated with a few examples of our recent work on two-dimensional electron gases and semiconductor quantum dots, on bulk GaAs and GaN, as well as on thin graphitic layers.

In order to understand the effect of the magnetic field on surface patterns on semi-conducting silicon melt in industrial Czochralski furnaces, we conducted a series of unsteady three-dimensional numerical simulations of silicon melt flow in a shallow annular pool under the axial magnetic field for the magnetic field strength from 0 to 0.1T. The pool is heated from the outer cylindrical wall and cooled at the inner wall. Bottom and top surfaces are adiabatic. When the magnetic field is weak, the simulation can predict various three-dimensional oscillatory flows depending on the radial temperature difference. With the much larger magnetic field, three-dimensional flow becomes axisymmetric steady flow. Details of flow and temperature disturbances are discussed and the critical magnetic field strengths for the onset of axisymmetric steady flow are determined.

Co uniform hierarchical microspheres were grown on a large scale at 200° by a simple hydrothermal method with the help of the surfactant polyvinylpyrrolidone (PVP). During the synthesis, the external magnetic field as a controlling factor assembled cobalt microspheres to form chain-like structures vertically on substrate. X-ray diffraction (XRD) and scanning electron microscopy (SEM) were used to characterize the product. The results indicate that three-dimensional (3D) Co microspheres are constructed by the cross-sectional nanoplatelets shape with a mean thickness of ~ 250 nm. The mechanism involved for the formation of the chain-like structures is discussed. The results of the vibrating sample magnetometer (VSM) show that the magnetic Co chains possess the saturation magnetization of 125.2 emu/g. Our work may shed some light on the design of other well-defined complex nanostructures, and as-grown architectures may have potential applications.

In order to discuss the stability of the gapless features in the spin liquid state against magnetic fields, we report results and analyses of low-temperature heat capacity measurements of EtMe₃Sb[Pd(dmit)₂]₂ under magnetic fields. The large upturn of $C_p{T}^{-1}$ at 0 T observed previously in EtMe₃Sb[Pd(dmit)₂]₂ can be attributed to the rotational tunneling of the methyl groups in the counter cations and this upturn is suppressed by applying magnetic fields. The phenomenological resemblance of the feature under magnetic field was confirmed by comparative discussion of heat capacity measurement of metal complex of [Cu(acac)(OCH${}_3)$]₂ having similar methyl groups. The gapless character evidenced by the finite electronic heat capacity coefficient, $\gamma$ was found to be retained upon applying 17 T in EtMe₃Sb[Pd(dmit)₂]₂, which means that spin liquid ground state is stable against high magnetic fields. The finite $\gamma$ in the spin liquid compounds is considered to be related to a kind of density of states in spin excitations rather than those determined by disorders such as spin glasses.

To solve the problems that the existing pressure generators require high mechanical excitation frequency, need large manufacturing cost and are hard to control, a kind of pressure generator with low-frequency based on magnetic fluid is proposed in this paper. Magnetic fluid possesses the advantages of both magnetism of solid magnetic material and fluidity of liquid. The first-order buoyancy of magnetic fluid changes with low frequency alternating magnetic field. Based on this, the superimposed magnetic field is generated by electrifying the conical solenoid coil connected with the long solenoid coil with magnetic core in parallel. Magnetic field and magnetic force in the model are analyzed, then the relationship between input current and output pressure is calculated. In addition, the experimental platform is built and the performance of the device is tested. The result shows that the pressure generator can produce the corresponding pressure signal according to the input current.

This paper reviews the fundamental issues associated with the magnetoplasmon excitations investigated in a semiconducting quantum wire characterized by a harmonic confining potential and subjected to an applied (perpendicular) magnetic field. We embark on the charge–density excitations in a two-subband model within the framework of Bohm–Pines's random-phase approximation. The problem involves two length scales: and , which characterize the strengths of the confinement and the magnetic field (B). Essentially, we focus on the device aspects of the intersubband collective (magnetoroton) excitation, which observes a negative group velocity between maxon and roton. Consequently, it leads to tachyon-like (superluminal) behavior without one's having to introduce the negative energies. Existence of the negative group velocity is a clear manifestation of a medium with population inversion brought about due to a metastable state caused by the magnetic field that satisfies the condition B > B_th; B_th being the threshold value below which the magnetoroton does not exist. The interest in negative group velocity is based on anomalous dispersion in a medium with inverted population, so that gain instead of absorption occurs at the frequencies of interest. A medium with an inverted population has the remarkable ability of amplifying a small optical signal of definite wavelength, i.e. it can serve as an active laser medium. An extensive scrutiny of the gain coefficient suggests an interesting and important application: The electronic device designed on the basis of such magnetoroton modes can act as an optical amplifier. Examining the magnetic field dependence of the life-time of magnetorotons leads us to infer that relatively smaller magnetic fields are optimal.

Voyager 2 discovered the unusual non-dipolar and non-axisymmetric magnetic fields of Uranus and Neptune (U/N) in the 1980s. The cause of the unique fields of U/N has been a major scientific question since then. The answer lies in physical properties of fluids that generate planetary magnetic fields by a dynamo: convecting, electrically-conducting fluids at high pressures P and temperatures T in planetary interiors. Fluids in planets at finite temperatures are degenerate condensed matter because of high densities: T/T_F ≪1, where T_F is Fermi temperature. For metallic fluid H, T/T_F≈0.015. The vast majority of measured properties of fluids at planetary P/Ts were made under dynamic compression to few 100 GPa (1 Mbar) and few 1000 K. Fluids in U/N are discussed in terms of experimental data. Major conclusions: (i) Magnetic fields of U/N are made by metallic fluid H at outer planetary radii in the vicinity of the crossover from insulating fluid H₂ to metallic fluid H. (ii) Because those fields are made near outer surfaces, it is reasonable to observe non-dipolar non-axisymmetric fields. (iii) A proposed mechanism for the existence of those fields is decoupling of global rotation of U/N from convective motions in their dynamos, unlike Earth with a dipolar field.

In this paper, we study the behavior of three-dimensional extremely-short optical pulses propagating in a system made of carbon nanotubes in the presence of an external magnetic field applied perpendicular both to the nanotube axis and to the direction of propagation of the pulse. The evolution of the electromagnetic field is classically derived on the basis of the Maxwell’s equations. The electronic system of carbon nanotubes is considered in the low-temperature approximation. Our analysis reveals the novel and unique ability of controlling the shape of propagating short optical pulses by tuning the intensity of the applied magnetic field. This effect paves the way for the possible development of innovative applications in optoelectronics.