Electron density diagnostics by use of a collisional excitation model of the oxygen VI doublet in the solar transition region

ABSTRACT

For spectral diagnostics in the solar transition region under the collision–equilibrium condition, the method for electron density diagnostics by the collisional excitation is discussed in this paper. By using observed signal ratio of spectral lines produced by the oxygen VI ion, we discuss the electron density by this method. We find that this method is valid for a large region of signal ratio (from 2.001 to 4.162). We obtain that the electron density increases with increasing signal ratio of the oxygen VI doublet, and the plasma has an electron density on the order of magnitude of 10⁶–10⁷?cm^?3. This discussion will be significant for study on spectral diagnostics of the solar transition region.     

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.     

Tangential System of Thomson Scattering for Tokamak T-15

Two systems of Thomson scattering diagnostics, with vertical and tangential probing, are used in the D-shaped plasma cross section in tokamak T-15. The tangential system allows measuring plasma temperature and density profiles along the major radius of the tokamak. This paper presents the tangential system project. The system is based on a Nd:YAG laser with wavelength of 1064 nm, pulse energy of 3 J, pulse duration of 10 ns, and repetition rate of 100 Hz. The chosen geometry allows collecting light from ten uniformly spaced points. Optimization of the registration system has been accomplished. The collected light will be transmitted through an optical fiber bundle with diameter of 3 mm and quartz fibers (numerical aperture is 0.22). Six-channel polychromators based on high-contrast interference filters have been chosen as spectral equipment. The radiation will be registered by avalanche photodiodes. The technique of electron temperature and density measurement is described, and estimation of its accuracy is carried out. The proposed system allows measuring the electron temperature with accuracy not worse than 10% within the range of 50 eV to 10 keV on the pinch edge over the internal contour, from 20 eV to 9 keV in the plasma central region, and from 2 eV to 400 eV on the pinch edge over the outer contour. The estimation is made for electron density of not less than 2.6 × 10¹³ cm^–3.     

Nanoflare heating model for collisionless solar corona

The problem of coronal heating remains one of the greatest unresolved problems in space science. Magnetic reconnection plays a significant role in heating the solar corona. When two oppositely directed magnetic fields come closer to form a current sheet, the current density of the plasma increases due to which magnetic reconnection and conversion of magnetic energy into thermal energy takes place. The present paper deals with a model for reconnection occurring in the solar corona under steady state in collisionless regime. The model predicts that reconnection time in the solar corona varies inversely with the cube of magnetic field and varies directly with the Lindquist number. Our analysis shows that reconnections are occurring within a time interval of 600 s in the solar corona, producing nanoflares in the energy range 10 ²¹–10 ²³ erg /s which matches with Yohkoh X-ray observations.     

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     

Thermal equilibrium criteria in a nitrogen plasma

A method for obtaining the lower electron density limit for LTE in a nitrogen plasma is described, whereby the experimentally determined ratio of the collisional-radiative ionization and recombination coefficients (S/α) is compared with the corresponding LTE value (Saha ratio). It is argued that if the electron density is increased from values of about 10¹⁶cm^-3, S/α should tend to the Saha ratio as LTE is approached. For NII and NIII spectral lines, this is found to happen at an electron density of a few times 10¹⁶cm^-3 when the electron temperature is about 3 eV, in good agreement with the LTE criterion of Griem.     

Spectroscopic diagnostics of carbon and aluminum laser-produced plasmas

VUV emission spectra of plasmas produced by focusing laser radiation with intensity of 10¹⁰–10¹¹ W/cm² on carbon and aluminum targets were studied. Using the partial local thermodynamic equilibrium model for an electron density exceeding 10¹⁷ cm^?3, the spectroscopic diagnostics and the analysis of ion composition of plasmas were carried out. The electron temperatures determined for carbon and aluminum plasmas from the ratio of intensities of ionic lines were found to be 8±3 eV and 11±4 eV, respectively. Stark broadening of aluminum lines was measured and parameters of electron broadening were determined. Using the spatially resolved measurement of Stark line broadening, the spatial density distribution and the law of electron gas expansion were found. The electron gas in the hot region of size 5 mm with an average density of (5±2) 10₁₇cm ^?3 experienced one-dimensional expansion according to the law 1/z ^1.1 with increasing distance z from the target.     

Diagnostics of the solar corona structure by the refraction effects on radio emission

The solar disc radio brightness distribution observed at RATAN-600 can be interpreted as the angular directivity of the disk center emission at viewing anglesΘ=arcsin(R/R₀) over an angular range of R<0.9R ₀ at several wavelengths in the 2.0–32 cm region. These spectra can be treated as an emission enhancement due to refraction effects in free-free corona emission. The model simulations show good agreement with the observations and lead to estimation of the electron density N_e=1·10 ⁹ cm^?3 and emission measureEM=6·10 ²⁶ cm^?5 for the quiet Sun.     

Dynamics of plasma corona of laser-irradiated spherical targets

The paper is devoted to an investigation of the formation and spreading of an inhomogeneous dense plasma heated by high-power laser radiation. The present status of the experimental and theoretical research in this field is analyzed. The “Kal'-mar” facility is used to study the dynamics of the plasma corona (electron density n_e ~ 10¹⁸–10²⁰ cm^-3), the law of motion of the critical (n_e ~ 10²¹ cm^-3) region of the plasma is established, and the dependence of the rate of compression of the shell targets on the initial parameters is determined. The electron temperature of the corona is measured with high temporal resolution in the course of the compression. A jetlike expansion of the “fast” ions is observed and investigated.     

Non-equilibrium ionization and electron density in the coronal plasma during solar flares

Summary The Li-like to He-like ion population ratio for calcium at the onset of solar flares is observed to be about 60% higher than in steady-state ionization balance. The measurement of the duration of this initial period of transient ionization and of the population ratios of adjacent ionization states allows an estimate of the electron density of the coronal plasma at flare onset. The density found in this study, within 1·10⁹ and 7·10⁹ cm⁻³ is comparable with the density typical of pre-flare active regions.     

On the origin of solar wind. Alfvén waves induced jump of coronal temperature

Absorption of Alfvén waves is considered to be the main mechanism of heating in the solar corona. It is concluded that the sharp increase of the plasma temperature by two orders of magnitude is related to a self-induced opacity with respect to Alfvén waves. The maximal frequency for propagation of Alfvén waves is determined by the strongly temperature dependent kinematic viscosity. In such a way the temperature jump is due to absorption of high frequency Alfvén waves in a narrow layer above the solar surface. It is calculated the power per unit area dissipated in this layer due to damping of Alfvén waves that blows up the plasma and gives birth to the solar wind. A model short wave-length (WKB) evaluation takes into account the 1/f² frequency dependence of the transversal magnetic field and velocity spectral densities. Such spectral densities agree with old magnetometric data taken by Voyager 1 and recent theoretical calculations in the framework of Langevin-Burgers MHD. The presented theory predicts existence of intensive high frequency MHD Alfvén waves in the cold layer beneath the corona. It is briefly discussed how this statement can be checked experimentally. It is demonstrated that the magnitude of the Alfvén waves generating random noise and the solar wind velocity can be expressed only in terms of satellite experimental data. It is advocated that investigation of properties of the solar surface as a random driver by optical methods is an important task for future solar physics.     

Study of the solar flare of December 16, 1988 on the basis of the 2.223-MeV γ line and initial characteristics of flare neutrons

The third burst of the solar flare of December 16, 1988 was investigated on the assumption of both Bessel and power spectra of the initial charged particles. Refined data on the flare-neutron-production cross sections were used and two different neutron source altitudes were considered. An increase in the solar plasma density under the flare region up 2 × 10¹⁷ cm^?3 has been found throughout the photosphere; in some cases, the plasma density increased to (3–6) × 10¹⁷ cm^?3 in the initial flare stages. The dynamics of the increase in the plasma density during γ emission has been traced. It is found that the particle spectrum changes from moderately hard to soft and then to hard during γ emission in both spectral representations.     

Diagnostics of High-Temperature,High-Density Plasma by Radiation Analysis

This article will be restricted to the diagnostics of laboratory plasmas having an average particle energy of higher than 30 eV per particle and a density of greater than 10¹⁹ particles per cm³. Common features of such plasmas related to applied spectroscopy are their complete ionization, the high excitation and ionization levels the particles, the large emission coefficients for continuum radiation over a wide spectral range from the X-ray region up to the infrared, their small size, high temperature and density gradients to the environment, and their transient nature.     

Optical spectra of hydrogen plasma at electron concentrations above 1019 cm−3

The optical spectra of a dense (nonideal) plasma formed in a pulsed discharge in a closed quartz capillary were studied. The emission spectra of pure hydrogen plasma at a temperature of 23000 K and an electron concentration of ～1.5×10¹⁹ cm^?3, twice the value achieved earlier, were obtained. The plasma diagnostics was carried out by spectroscopic methods taking into account the radial inhomogeneity of the plasma column. The spectral intensity measured in the Balmer region (300–800 nm) was found to be lower than that calculated by the model of weakly nonideal plasma, an effect not observed at lower densities. Possible reasons for the discrepancy between the experiment and the calculation were considered. One of them being the specific density effect of a relative rise in plasma transmission with increasing density.     

Calibration of the X-Ray spectroheliograph Mg XII for the 0.84 nm spectral line for the TESIS experiment

The spectroheliograph for monochromatic imaging of the solar corona at the 0.84 nm resonance line of a Mg XII ion is a part of the TESIS instrumentation onboard the CORONAS-PHOTON satellite. The main optical elements of the spectroheliograph are the focusing crystalline mirror and imaging detector based on a CCD array. The optical scheme of the spectroheliograph, procedure, and results of calibrations of the optical elements within the working spectral range are presented. Diffraction efficiency and the rocking curve of the crystalline mirror, sensitivity, and radiation hardness of the detector were measured. It was found that the diffraction efficiency is 10%, the width of the rocking curve is ～3′, the detector sensitivity is 31 ADC units per photon, and the radiation hardness is better than 10⁷ rad within the working spectral range.     

Thin Film Solar Cell Based on ZnSnN2/SnO Heterojunction

In this article, we report the growth of zinc‐tin nitride (ZnSnN₂) thin films as a potential absorber for photovoltaic applications by fabricating a heterojunction of n‐ZnSnN₂/p‐SnO. The performance of the heterojunction has been monitored through selective deposition of top electrode with different materials (Ni/Au or Al). The electron‐transfer process from the ZnSnN₂ layer to the cathode is facilitated by selecting metal electrode with relatively low work function, which also boosts up the electron injection or/and extraction. The diode exhibits a good J–V response in the dark with a rectification ratio of 3 × 10³ at 1.0 V and an ideality factor of 4.2 in particular with Al as the top electrode. Under illumination, the heterostructure solar cell demonstrates a power conversion efficiency of ≈0.37% with an open circuit voltage of 0.25 V and a short circuit current density of 4.16 mA cm^?2. The prime strategies, on how to improve solar cell efficiency concerning band offsets and band alignment engineering are also discussed.     

Modernized active spectroscopic diagnostics (CXRS) of the T-10 tokamak

This work presents the results of modernization of the CXRS (charge exchange recombination spectroscopy) diagnostics [1] at the T-10 tokamak. The relevance of this work is due to the importance of measurements of the ion temperature and nuclei density of the working gas and impurities for analysis of transport processes in the plasma ion component. Measurements of radial profiles of the ion temperature are extremely important for investigating the geodesic acoustic mode behavior which is conducted at the T-10 [2]. The modernized scheme of CXRS measurements, as well as the design and operational features of the spectrometer created for the new diagnostics, is described. Principles of data recording and further processing are considered in detail; attention is given to the problem of calibration of the whole complex of equipment. The performed changes in diagnostics allow the measurements to be taken simultaneously in three spectral intervals: in the region of the beam line H_α, the CXRS line of carbon ion C⁵⁺, and the CXRS line of one of the hydrogen-like ions: He¹⁺, Li²⁺, N⁶⁺, O⁷⁺ or Ne⁹⁺. This makes it possible to measure the density profiles of two plasma impurities simultaneously, as well as the ion temperature from CXRS lines of different elements. The modernized diagnostics significantly broadens the possibilities of studying the physics of transport processes and quasi-coherent modes of plasma oscillations at the T-10.     

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.     

Investigation of the solar transition layer and corona by the method of imaging XUV spectroscopy in the terek and res experiments on board the KORONAS-I satellite

The method of imaging XUV spectroscopy was used to study plasma in the transition layer and inner corona of the Sun with temperatures 10⁵–10⁷ K in the TEREK and RES experiments on board KORONAS-I. The observations were carried out in the period from March 12 to July 5, 1994. The spectral images and their correlation with the YOHKOH X-ray images and groundbased observations are important for the study of the physical conditions and modeling of the bulk processes in the quiet Sun plasma, including active regions, corona holes, and overlimb structures.     

Role of equilibrium plasma flow on damping of slow MHD waves

In the solar corona waves and oscillatory activities are observed with modern imaging and spectral instruments. These oscillations are interpreted as slow magneto-acoustic waves excited impulsively in coronal loops. This study explores the effect of steady plasma flow on the dissipation of slow magneto-acoustic waves in the solar coronal loops permeated by uniform magnetic field. We have investigated the damping of slow waves in the coronal plasma taking into account viscosity and thermal conductivity as dissipative processes. On solving the dispersion relation it is found that the presence of plasma flow influences the characteristics of wave propagation and dissipation. We have shown that the time damping of slow waves exhibits varying behavior depending upon the physical parameters of the loop. The wave energy flux associated with slow magnetoacoustic waves turns out to be of the order of 10⁶ erg cm⁻² s⁻¹ which is high enough to replace the energy lost through optically thin coronal emission and the thermal conduction below to the transition region.