Investigation of Vector Perturbations in a Radiation-Dominated Cosmological Plasma

Based on the Maxwell–Einstein equations together with hydrodynamic plasma equations derived with allowance for Compton scattering, vector perturbations are examined for a homogeneous isotropic spatially-flat model of the Universe. The magnetic field strength generated by these vector perturbations in the radiation-dominated stage of evolution of the Universe is calculated.     

Kinetics of interacting gravitational and electromagnetic perturbations in cosmological plasma

The system of Einstein-Maxwell equations and a kinetic equation with a model collision integral for the cosmological plasma is used to study the behavior of gravitational and electromagnetic perturbations in the radiation-dominated stage of expansion of the universe. It is shown that gravitational perturbations are capable of generating electromagnetic fields in the cosmological plasma.Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Fizika, No. 1, pp. 91–96, January, 1992.     

Joint behavior of longitudinal electromagnetic waves and scalar gravitational disturbances in the cosmological plasma with allowance for electron-photon collisions

The electric charge density induced by scalar gravitational perturbations in the radiation-dominated stage of the expansion of the universe is calculated on the basis of an investigation of the combined system of Einstein, Maxwell, and kinetic equations for a cosmological plasma with a model collision integral.Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Fizika, No. 2, pp. 97–100, February, 1992.     

Generation of longitudinal plasma oscillations by gravitational perturbations in an isotropic universe

The electric charge density induced by scalar gravitational perturbations in the lepton and radiation-dominated stages of the expansion of the universe is calculated. It is shown that the formation of clusters of matter is accompanied in the radiation-dominated stage by a build-up of positive charge in the central regions of the cluster. The charge-mass relation of the clusters is calculated.Translated from Izvestiya Vysshkikh Uchebnykh Zavedenii, Fizika, No. 5, pp. 52–57, May, 1986.     

Propagation of transverse electromagnetic waves with gravitational perturbations in an isotropic universe

The combined behavior of gravitational and electromagnetic perturbations in the radiation-dominated plasma of an isotropic universe is considered. It is shown that transverse electromagnetic waves and vector and tensor gravitational perturbations are independent of one another. The propagation of transverse electromagnetic waves during the lepton and radiation-dominated phases is determined. It is shown that the gravitational perturbations help to excite longitudinal electromagnetic fields in the radiation-dominated plasma.Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Fizika, No. 12, pp. 49–54, December, 1985.     

An optimized solenoidal head radiofrequency coil for low-field magnetic resonance imaging

Applications of low-field magnetic resonance imaging (MRI) systems (<0.3 T) are limited due to the signal-to-noise ratio (SNR) being lower than that provided by systems based on superconductive magnets (≥1.5 T). Therefore, the design of radiofrequency (RF) coils for low-field MRI requires careful consideration as significant gains in SNR can be achieved with the proper design of the RF coil. This article describes an analytical method for the optimization of solenoidal coils. Coil and sample losses are analyzed to provide maximum SNR and optimum B₁ field homogeneity. The calculations are performed for solenoidal coils optimized for the human head at 0.2 T, but the method could also be applied to any solenoidal coil for imaging other anatomical regions at low field. Several coils were constructed to compare experimental and theoretical results. A head magnetic resonance image obtained at 0.2 T with the optimum design is presented.     

Confinement physics for thermal, neutral, high-charge-state plasmas in nested-well solenoidal traps

A theoretical study is presented which indicates that it is possible to confine a neutral plasma using static electric and solenoidal magnetic fields. The plasma consists of equal temperature electrons and highly stripped ions. The solenoidal magnetic field provides radial confinement, while the electric field, which produces an axial nested-well potential profile, provides axial confinement. A self-consistent, multidimensional numerical solution for the electric potential is obtained, and a fully kinetic theoretical treatment on axial transport is used to determine an axial confinement time scale. The effect on confinement of the presence of a radial electric field is explored with the use of ion trajectory calculations. A thermal, neutral, high-charge-state plasma confined in a nested-well trap opens new possibilities for fundamental studies on plasma recombination and cross-field transport processes under highly controlled conditions.     

Coherence and oscillations of cosmic neutrinos

For cosmic neutrinos we study the conditions and the effects of the coherence loss as well as coherent broadening of the spectrum. We evaluate the width of the neutrino wavepacket produced by charged particles under various circumstances: in an interaction-free environment, in a radiation-dominated medium (typical of the sources of the gamma ray bursts) and in the presence of a magnetic field. The effect of the magnetic field on the wavepacket size appears to be more important than the scattering. If the magnetic field at the source is larger than 10 Gauss, the coherence of neutrinos will be lost while traveling over cosmological distances. Various applications of these results have been considered. We find that for large magnetic fields (B>10⁹ Gauss) and high energies (E_ν>PeV), “coherent broadening” can modify the energy spectrum of neutrinos. In the coherent case, averaging out the oscillatory terms of the probabilities does not induce any statistical uncertainty beyond what expected in the absence of these terms. A deviation from the standard quantum mechanics that preserves average energy and unitarity cannot alter the picture.     

行波管中静态轨迹的研究

研究了行波管中均匀聚焦磁场和周期永磁聚焦磁场对轨迹波动的影响。推导了这两种磁场下轨迹波动周期和幅值,讨论了磁场强度对轨迹的影响。解释了聚焦磁场存在小的波动的原因,并且通过计算得出小波动的周期为磁场周期的1/2,揭示了在周期永磁聚焦磁场下,电子轨迹近似等效于周期为周期永磁聚焦磁场1/2的小波动和均匀磁场形成的波动轨迹的叠加。利用电子科技大学编写的微波管模拟套装中的3维注-波互作用模块进行了静态轨迹计算,验证了理论推导。     

Density perturbations in a cosmological de Donder gauge

Density perturbations are considered during the radiation-dominated and the dust-dominated periods of the expanding universe. The perturbations are taken to have spherical symmetry and the investigation is carried out in the de Donder gauge. In order to guarantee the energy-momentum conservation of the perturbation in the de Donder gauge a compatibility condition is obtained. Equations for the propagation of a spherically symmetric perturbation in linear approximation on a FRW cosmological background are presented. It turns out that the evolutiontendency of the formation is mainly predicted by the state of the cosmic background. A radiation-dominated universe does not stimulate growth processes; the perturbation will be in a frozen state or it will diffuse. It is found that the dust-dominated universe stimulates the perturbation mass to grow. The rate of this cosmic affected growing process is proportional toR ^–1 (R being the scale factor of the universe), so that it seems that almost all galaxies were formed at the beginning of the present dust-dominated era.     

Influence of the intrinsic magnetic moment of an electron on the filling of energy levels of a nonrelativistic degenerate electron gas in a quantizing magnetic field

The effect of a quantizing magnetic field on the filling of energy subbands of a degenerate nonrelativistic electron gas, whose magnetic moments are parallel and antiparallel to the direction of the field, is studied. Calculations are made under the assumption that the Fermi kinetic energy of the electron system increases as a result of Pauli's paramagnetism as compared to the kinetic energy calculated without taking this effect into account. Numerical values of the electron concentration are calculated as a function of the magnetic moment direction for magnetic fields under which the electrons are in states with given numbers of the Landau quantum level.A. S. Pushkin State Education Institute, Brest. Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Fizika, No. 6, pp. 9–13, June, 1992.     

Threshold Frequency of Helical Electron–Hole Plasma Instability

Experimental evidence on the dependence of the threshold frequency of silicon oscillistors on the threshold electric field strength, magnetic induction, temperature, and injecting-contact separation is presented. In the temperature interval, where the weak magnetic field criterion is roughly satisfied, the experimental results are shown to be adequately explained by the classical theory of the bulk helical instability of an extrinsic plasma. The threshold frequency in this temperature interval is determined by the sum of two components. One component is due to the ambipolar drift of helical plasma perturbations, and the other results from the presence of the charge-carrier concentration gradient in a direction normal to the vectors of the electric field strength and magnetic induction. In short oscillistors (0.85·10^–3, 2.38·10^–3 m) at 77 K, a semiconductor plasma, wherein the helical instability is excited, approximates an intrinsic plasma, and the threshold frequency is determined by the rotation rate of helical perturbations.     

Exact Perturbations for Inflation with Smooth Exit

Toy models for the Hubble rate or the scalar field potential have been used to analyze the amplification of scalar perturbations through a smooth transition from inflation to the radiation era. We use a Hubble rate that arises consistently from a decaying vacuum cosmology, which evolves smoothly from nearly de Sitter inflation to radiation domination. We find exact solutions for super-horizon perturbations (scalar and tensor), and for sub-horizon perturbations in the vacuum- and radiation-dominated eras. The standard conserved quantity for super-horizon scalar perturbations is exactly constant for the growing modes, and zero for the decaying modes.     

Stationary Kepler orbits of the electron with velocity-dependent perturbations — classical quantization

In this paper the evolution of Kepler orbits generated by velocity-dependent perturbations is discussed. It is found that in the presence of oscillatory perturbations, of oscillation frequency proportional to the kinetic energy of the moving particle, a discrete set of stationary orbits exists. If the coefficient of proportionality in the frequency—kinetic energy relation is the Planck constant, the orbits are the same as those given by Bohr's quantum postulates. The conclusion is drawn that the Schrödinger wave equation describes, in hidden form, velocity-dependent oscillatory perturbations superimposed upon the basic motion of an electron and has nothing in common with the basic trajectory of the motion.     

Development of a 2 MW relativistic backward wave oscillator

In this paper, a high power relativistic backward wave oscillator (BWO) experiment is reported. A 230 keV, 2 kA, 150 ns relativistic electron beam is generated using a Marx generator. The beam is then injected into a hollow rippled wall metallic cylindrical tube that forms a slow wave structure. The beam is guided using an axial pulsed magnetic field having a peak value 1 T and duration 1 ms. The field is generated by the discharge of a capacitor bank into a solenoidal coil. A synchronization circuit ensures the generation of the electron beam at the instant when the axial magnetic field attains its peak value. The beam interacts with the SWS modes and generates microwaves due to Cherenkov interaction. Estimated power of 2 MW in TM₀₁ mode is observed.      

Relaxation of powerful electron beam in air in a strong inhomogeneous magnetic field

Numerical calculations of the relaxation of a powerful (0.6 MW) high-energy (0.2 MeV) beam in air (P=1 atm) in a strong solenoidal magnetic field are undertaken by the combined-code method, including the Monte Carlo method for the calculation of beam evolution, the characteristic method for the calculation of the divergence of the radiant flux, and the Pismen-Rekford method for the calculation of the temperature field of air. The heat-liberation zone and intensity in the chamber are calculated, as well as the air temperature and the beam bremsstrahlung, and the results are compared with experiment.Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Fizika, No. 7, pp. 69–73, July, 1990.     

Charge and current neutralization of an ion-beam pulse propagating in a background plasma along a solenoidal magnetic field

The analytical studies show that the application of a small solenoidal magnetic field can drastically change the self-magnetic and self-electric fields of the beam pulse propagating in a background plasma. Theory predicts that when omega_{ce} approximately omega_{pe}beta_{b}, where omega_{ce} is the electron gyrofrequency, omega_{pe} is the electron plasma frequency, and beta_{b} is the ion-beam velocity relative to the speed of light, there is a sizable enhancement of the self-electric and self-magnetic fields due to the dynamo effect. Furthermore, the combined ion-beam-plasma system acts as a paramagnetic medium; i.e., the solenoidal magnetic field inside the beam pulse is enhanced.     

Gravitational instability of the primordial plasma: Anisotropic evolution of structure seeds

We study how the presence of a background magnetic field, of intensity compatible with current observation constraints, affects the linear evolution of cosmological density perturbations at scales below the Hubble radius. The magnetic field provides an additional pressure that can prevent the growth of a given perturbation; however, the magnetic pressure is confined only to the plane orthogonal the field. As a result, the “Jeans length” of the system not only depends on the wavelength of the fluctuation but also on its direction, and the perturbative evolution is anisotropic. We derive this result analytically and back it up with direct numerical integration of the relevant ideal magnetohydrodynamics equations during the matter-dominated era. Before recombination, the kinetic pressure dominates and the perturbations evolve in the standard way, whereas after that time magnetic pressure dominates and we observe the anisotropic evolution. We quantify this effect by estimating the eccentricity ?   of a Gaussian perturbation in the coordinate space that was spherically symmetric at recombination. For a perturbations at the sub-galactic scale, we find that ?=0.7$?=0.7$ at z=10$z=10$ taking the background magnetic field of order 10⁻⁹${10}^{-9}$ gauss.