Stability of electrostatic ion cyclotron waves in a multi-ion plasma

We have studied the stability of the electrostatic ion cyclotron wave in a plasma consisting of isotropic hydrogen ions (H⁺) and temperature-anisotropic positively (O⁺) and negatively (O⁻) charged oxygen ions, with the electrons drifting parallel to the magnetic field. Analytical expressions have been derived for the frequency and growth/damping rate of ion cyclotron waves around the first harmonic of both hydrogen and oxygen ion gyrofrequencies. We find that the frequencies and growth/damping rates are dependent on the densities and temperatures of all species of ions. A detailed numerical study, for parameters relevant to comet Halley, shows that the growth rate is dependent on the magnitude of the frequency. The ion cyclotron waves are driven by the electron drift parallel to the magnetic field; the temperature anisotropy of the oxygen ions only slightly enhance the growth rates for small values of temperature anisotropies. A simple explanation, in terms of wave exponentiation times, is offered for the absence of electrostatic ion cyclotron waves in the multi-ion plasma of comet Halley.     

Coherent backscattering of electromagnetic waves in a magnetised plasma

Summary A microwave coherent backscattering experiment has been carried out on Mirabelle, a weakly ionised plasma device, with the objective of measuring the electron density fluctuation level. The experiment is a preliminary step in order to prepare the detection system for a microwave stimulated backscattering experiment. The incident electromagnetic wave is focused in front of a plane grid which excites ion acoustic or electron Bernstein waves inducing fluctuations in the plasma. The backscattering signal is collected by the launching circuit and detected by homodyne mixing. The typical ratio of the scattered power to the incident power is about 10⁻¹² and the relative density fluctuations are of the order of δn _e/n _e=10⁻³ against a background electron density ofn _e=1–5·10⁹ cm⁻³. The backscattering measurement is compared with Langmuir probe measurements. The spectral width of the backscattered signal has also been studied, by taking into account effects due to the incident wave focusing and plasma wave damping. The authors of this paper have agreed to not receive the proofs for correction     

Energy release in corona magnetic loops

It is found that thin magnetic tubes of radius about 10⁷-10⁸ cm and longitudinal current 10¹¹-10¹² A can be generated under the conditions of convective flows in the solar photosphere. Moreover, the so-called “magnetic holes”, cylindrical magnetic structures with magnetic field decreasing towards the center, can be formed in divergent convective (Evershed) flows. It is shown that the steady-state Joule energy release (dissipation) at the photospheric footpoints of a magnetic tube increase towards the tube periphery in the upper photosphere and can exceed the optical radiation losses. In particular, this can lead to the occurrence of magnetic tubes with hot external envelopes. We consider two models of magnetic flaring loops in the active region. One model describes the explosive energy release in an individual loop caused by the penetration of the dense partially ionized plasma of a prominence into the magnetic tube (in the upper part of the loop) due to flute instability or the penetration of the surrounding chromospheric plasma (in the chromospheric part of the loop). The inflow of these plasmas destroys the force-free structure of the magnetic tube and switches on an efficient mechanism of energy release due to ion-atom collisions in a non-steady-state plasma. We studied the dynamics of the joule energy release in such processes. The second model of flaring energy release is based on the global approach in the study of the dynamics and energetics of solar active regions with allowance for their complex self-consistent evolution. The structure of the magnetic field of an active region was represented as an ensemble of inductively coupled current-carrying magnetic loops interacting with each other. Each loop, in turn, was simulated by an equivalent electric circuit with variable parameters as a function of the shape, scale, and position of the loop in the ensemble as well as of the plasma temperature and density in the magnetic tube. Using this model, we showed that a rising magnetic loop can cause thermal flare-like heating of one loop and cooling of other loops in the ensemble. Institute of Applied Physics, Russian Academy of Sciences, Nizhny Novgorod. Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika, Vol. 40, Nos. 1–2, pp. 176–212, January–February, 1997.     

Normal modes of a resistive nonuniform plasma

The propagation and dissipation properties of magnetohydrodynamic waves in a nonuniform, highlyconducting plasma, is investigated with a normal mode approach. The interaction between the perturbation and the non-uniform supporting medium is analyzed as the main mechanism able to produce the small scale spatial structure necessary to dissipate efficiently the wave energy. Two fundamental classes of modes are found, characterized by their resistive or ideal asymptotic behavior; the damping rates are shown to be orders of magnitude larger than those obtained when the plasma is perfectly homogeneous, and an application to the problem of solar coronal heating is discussed.Astronomia e Scienza dello spazio, Universitá di Firenze, Italy. Observatoire de Paris-Meudon (DESPA), France. Published in Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika, Vol. 37, No. 5, pp. 563–579, May, 1994.     

Conductivity tensor of the coronal plasma

We study the plasma conductivity within the framework of the magnetohydrodynamic approximation under conditions typical of the coronas of the Sun and stars of the late spectral classes. The problem of finding the elements of the plasma conductivity tensor is reduced to derivation of approximate formulas and numerical values. It is shown that two regimes of dissipation of the current running across the magnetic field can be realized in the corona, namely, one due to the friction of the ion and neutral plasma components (Cowling conductivity) and the other, due to the friction of two different ion components. The first regime is realized in the larger part of the lower corona, whereas the condition for realization of the second regime, i.e., B/n _e < 10⁻⁹ G·cm³, where B is the magnetic field and ne is the electron number density, can be satisfied in the base of the solar corona or in coronal streamers. In the second regime, the rate of the transverse-current dissipation increases tenfold compared with the hydrogen plasma. The longitudinal and Hall components of the conductivity tensor differ only slightly from their values for the electron–proton plasma. The paper draws attention to the fact that along with the momentum exchange due to the charge exchange, the momentum exchange due to ionization and recombination during electron collisions plays a significant part in the friction of neutral and ionized hydrogen atoms.     

Signatures of the neutrino thermal history in the spectrum of primordial gravitational waves

In this paper we study the effect of the anisotropic stress generated by neutrinos on the propagation of primordial cosmological gravitational waves. The presence of anisotropic stress, like the one generated by free-streaming neutrinos, partially absorbs the gravitational waves (GWs) propagating across the Universe. We find that in the standard case of three neutrino families, 22% of the intensity of the wave is absorbed, in fair agreement with previous studies. We have also calculated the maximum possible amount of damping, corresponding to the case of a flat Universe completely dominated by ultrarelativistic collisionless particles. In this case 43% of the intensity of the wave is absorbed. Finally, we have taken into account the effect of collisions, using a simple form for the collision term parameterized by the mean time between interactions, that allows to go smoothly from the case of a tightly coupled fluid to that of a collisionless gas. The dependence of the absorption on the neutrino energy density and on the effectiveness of the interactions opens the interesting possibility of observing spectral features related to particular events in the thermal history of the Universe, like neutrino decoupling and electron–positron annihilation, both occurring at T ~ 1  MeV. GWS entering the horizon at that time will have today a frequency ν ~ 10⁻⁹ Hz, a region that is going to be probed by Pulsar Timing Arrays.     

Return current instability and its effects on beam-plasma system

The return current induced in a plasma by a relativisitc electron beam generates a new electron-ion two-stream instability (return current instability). Although the effect of these currents on the beam-plasma e-e instability is negligible, there exists a range of wave numbers which is unstable only to return current (RC) instability and not to e-e instability. The electromagnetic waves propagating along the direction of the external magnetic field, in which the plasma is immersed, are stabilized by these currents but the e.m. waves with frequencies,ω ²≪Ω _e ² ≪ω _pe ² (Ω _e andω _pe being cyclotron and plasma frequency for the electrons of the plasma respectively) propagating transverse to the magnetic field get destabilized. Heuristic estimates of plasma heating, due to RC instability and due to decay of ion-acoustic turbulence generated by the return current, are made. The fastest time scale on which the return current delivers energy to the plasma due to the scattering of ion-sound waves by the electrons can be ∼ω _pi ⁻¹ (ω _pi being the plasma frequency for the ions).     

Generation of coherent thermal phonons in amorphous dielectrics at room temperature induced by four-photon interaction

Resonant responses of Mandelshtam-Brillouin scattering from longitudinal and transverse acoustic waves at frequencies of ν _LS = ±1.15 cm⁻¹ and ν _TS = ±0.7 cm⁻¹, respectively, and at frequency of ν _SS = ν _TS $ \sqrt 3 $ \sqrt 3 = ±0.43 cm⁻¹ were detected in K8 optical glass at room temperature using four-photon spectroscopy. We attribute this effect to the induced generation of a second sound wave (coherent thermal phonons). The mechanisms of generation and the possibility of practical application of the observed effect for express diagnostics of the quality of transparent materials are discussed.     

Influence of Dissipative Processes on the Propagation of Excitons and Plasmons in Layered Periodic Structures

We study propagation of electromagnetic waves in an unbounded periodic semiconductor-dielectric structure. The frequency range for which optical phonons propagate in the dielectric layer is considered. It is shown that the plasma and exciton waves have a specific band structure of the spectrum. The influence of dissipation on the phase velocity of propagation of the waves of these types is studied. It is found that slow waves with phase velocityies about 10⁸ cm/s can exist in the considered layered-periodic structure. __________ Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika, Vol. 48, No. 4, pp. 349–357, April 2005.     

Surfing and generation of cosmic rays in relativistic shock waves

We consider the problem of cosmic-ray generation through the surfing acceleration of charged particles in relativistic magnetosonic shock waves (the branch of fast magnetic sound) propagating in magnetized space plasmas. The dependence of the particle surfing acceleration efficiency on the angle θ _Bn between the normal to the shock front plane and the magnetic field vector in the plasma upstream of the shock is analyzed in detail. We show that for angles satisfying the condition χ = βΓ tan θ _Bn ⩾ 1, where β = U/c, Γ = (1 − β)^{2 −1/2}, U is the shock velocity, and c is the speed of light, the particles can theoretically be accelerated through surfing for an unlimited time and can gain an unlimited energy. For angles satisfying the condition χ < 1, the kinetic energy ℰ of the particles is limited by ℰ = 2mc ²χ²/(1 − χ²) (m is the particle rest mass). Our main conclusion is that the generation of cosmic rays through the surfing acceleration of particles in the front of a relativistic shock wave for Γ ≫ 1 is also efficient when the angle θ _Bn is very small, i.e., it differs significantly from a right angle. Estimates for the energies of particles accelerated through surfing in relativistic jets are provided.     

Experiments on two-step heating of a dense plasma in the GOL-3 facility

This paper presents the results of experiments on two-stage heating of a dense plasma by a relativistic electron beam in the GOL-3 facility. A dense plasma with a length of about a meter and a hydrogen density up to 10¹⁷ cm⁻³ was created in the main plasma, whose density was 10¹⁵ cm⁻³. In the process of interacting with the plasma, the electron beam (1 MeV, 40 kA, 4 μs) imparts its energy to the electrons of the main plasma through collective effects. The heated electrons, as they disperse along the magnetic field lines, in turn reach the region of dense plasma and impart their energy to it by pairwise collisions. Estimates based on experimental data are given for the parameters of the flux of hot plasma electrons, the energy released in the dense plasma, and the energy balance of the beam-plasma system. The paper discusses the dynamics of the plasma, which is inhomogeneous in density and temperature, including the appearance of pressure waves. Zh. éksp. Teor. Fiz. 113, 897–917 (March 1998)     

Efficiency of electron acceleration by shock waves in the solar corona according to observational data on the fine structure of type II radio bursts

Herringbone bursts (HB-bursts) are the type III-like fine structure in type II bursts of solar radio emission and are usually interpreted as plasma radiation arising from fast electrons accelerated by shock waves in the solar corona. In general outline, the radiation mechanism of HB-bursts is similar to that of type III bursts. However, HB-bursts have brightness temperatures that are about an order of magnitude higher than those of type III bursts. The frequency drift of BH-bursts is about two or three times lower than that for type III bursts. All this shows that the fast-electron beams responsible for HB-bursts and type III bursts differ markedly in their parameters. We calculated expected brightness temperatures of HB-bursts at the fundamental and second harmonic and compared our results with Culgoora radiometer and radioheliograph data and Tremsdorf spectrograph data in order to estimate parameters of fast-electron beams generating HB-bursts. We found that the observed brightness temperatures of HB-bursts give velocities of fast electrons accelerated by shock waves within the limits (0.02–0.17)c. These velocities are several times lower than those for type III bursts (0.15–0.5)c. The density of the fast electrons responsible for HB-bursts is in the interval 3·10⁻⁶ <n_b/n<6·10⁻⁵, which exceeds by 1–2 orders of magnitude the relative densities in type III sources. This gives a clue to understanding the markedly higher brightness temperatures of HB-bursts compared to those of type III bursts. We concluded that the parameters obtained for the agent exciting HB-bursts favor of turbulence mechanisms of electron acceleration by shock waves in the solar corona. Institute of Applied Physics, Russian Academy of Sciences, Nizhny Novgorod, Russia; Astrophysical Institute, Potsdam, Germany. Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika, Vol. 41, No. 2, pp. 164–176, February, 1998.     

“Quasi-Planck” spectra of capillary turbulence on the surface of liquid hydrogen

We report the first observation of “quasi-Planck” spectra of capillary turbulence on the surface of liquid hydrogen in the dissipation domain. Capillary waves have been driven by low-frequency random force. We have observed that the frequency spectrum of surface elevation changes its dependence from power-like 〈|η_ω²|〉 ∼ ω^−2,8 at middle-frequency domain to “quasi-Planck” distribution ∼e ^ω/ω _d at higher frequencies. The frequency ω _d is proportional to the boundary frequency between inertial interval and dissipation domain and it is scaled up with the increase of driving force.     

Model of pulsed electric discharge expansion in dense gas taking into account electron and radiative thermal conductivities. II. Energy balance and equation

Using an ionization sensor, it was found that weakly ionized plasma with an ionization degree larger than 10⁻⁶ is formed under exposure to UV radiation of a high-current pulsed electric discharge in gas (air, nitrogen, xenon, and krypton) at atmospheric pressure at a distance of ∼1.2–2.5 cm from the discharge boundary. It was shown that the structure of such discharge includes, in addition to the discharge channel, a dense shell and a shock wave, also a region of weakly ionized and excited gas before the shock wave front. The mechanism of discharge expansion in dense gas is ionization and heating of gas involved in the discharge due to absorption of the UV energy flux from the discharge channel and the flux of the thermal energy transferred from the discharge channel to the discharge shell due to electron thermal conductivity.     

Probability of the occurrence of freak waves

The statistics of the occurrence of freak waves on a surface of an ideal heavy liquid is studied. The freak (rogue, extreme) waves arise in the course of evolution of a statistically homogeneous random Gaussian wave field. The mean steepness of initial data varies from small (μ² = 1.54 × 10⁻³) to moderate (μ² = 3.08 × 10⁻³) values. The frequency of the occurrence of extreme waves decreases with an increase in the spectral width of the initial distribution, but remains relatively high even for broad spectra (Δ _k /Δ ∼ 1).     

Strength properties of an aluminum melt at extremely high tension rates under the action of femtosecond laser pulses

The dynamics of the melting of a surface nanolayer and the formation of thermal and shock waves in metals irradiated by femtosecond laser pulses has been investigated both experimentally and theoretically. A new experimental-computational method has been implemented to determine the parameters of laser-induced shock waves in metallic films. Data on the strength properties of the condensed phase in aluminum films at an extremely high strain rate ($ \dot V $ \dot V /V ∼ 10⁹ s⁻¹)under the action of a laser-induced shock wave have been obtained.     

On ejection of solar plasma enriched with 3He and Fe I at boundaries of coronal holes

The spectra and spectroheliograms in the He I λ = 1083.03 nm IR-line obtained with the horizontal solar telescope of the Sternberg State Astronomical Institute (SSAI) of Moscow State University are analyzed for the purpose of studying the increased solar activity at the boundaries of coronal holes. Our observations demonstrate plasma flux intensification at the boundary separating a coronal hole and a bipolar active region. In this case, the spectra in the vicinity of the He I λ = 1083.03 nm line point to a significant intensification in the lines of light isotope ³He I λ = 1083.168 nm and Fe I λ = 1082.837 nm. Acceleration of solar plasma fluxes at the coronal hole boundary in the immediate vicinity of an active region seems to be the result of reconnection of bipolar structure magnetic fields in the active region and a unipolar field of the coronal hole. The nature of ³He and Fe I particle enrichment in upward fluxes at the coronal hole boundaries is discussed. Original Russian Text ? L.M. Kozlova, B.V. Somov, 2009, published in Vestnik Moskovskogo Universiteta. Fizika, 2009, No. 3, pp. 94–98.     

Gravitational wave generation in power-law inflationary models

We investigate the generation of gravitational waves in power-law inflationary models. The energy spectrum of the gravitational waves is calculated using the method of continuous Bogoliubov coefficients. We show that, by looking at the interval of frequencies between 10⁻⁵ and 10⁵ Hz and also at the GHz range, important information can be obtained, both about the inflationary period itself and about the thermalization regime between the end of inflation and the beginning of the radiation-dominated era. We thus deem the development of gravitational wave detectors, covering the MHz/GHz range of frequencies, to be an important task for the future.     

Dispersion Relations for Drift-Alfvén and Drift-Acoustic Waves in Arbitrary Directions

A dispersion equation for low-frequency waves in a fully ionized plasma with slowly varying density and magnetic field is derived from the two-fluid equations. The solutions are discussed in several limiting cases. Phase-velocity and refractive index surfaces are presented for the fast and slow magneto-acoustic waves and for the shear-Alfvén wave, influenced by the inhomogeneity drifts.