Stark widths of Ar III spectral lines in the atmospheres of subdwarf B stars

Using semiclassical perturbation approach in impact approximation, we have calculated Stark widths for 32 spectral lines of doubly charged argon (Ar III). Oscillator strengths are calculated using Hartree–Fock method with relativistic correction (HFR) and an atomic model including 17 configurations. Energy levels are taken from NIST database. For perturbing levels for which the corresponding energy does not exist in NIST database, the calculated energies are used. Our widths are compared with the experimental results. The results presented here are of interest for modelling and investigation of stellar atmospheres since argon in different ionization stages is observed in many astrophysical objects. Finally, the importance of Stark broadening mechanism is studied in the atmospheric conditions of sdB stars. Electron impact Stark widths are compared to thermal Doppler widths as a function of temperature and optical depth of atmospheric layers.     

Stochastic processes for line shapes and intensities

Stochastic processes provide flexible and fast calculations for modeling dynamical interactions between an atom and charged particles. We use a stochastic renewal process for the plasma microfield being the cause of Stark broadening. The accuracy and improvement possibilities of Lyman profiles calculations with a renewal process are analyzed by comparing to ab initio simulations for ion broadening only. Stochastic processes may also be applied to out of equilibrium plasmas. We present our first results for the effect of Langmuir waves on a line broadened by electrons only, and for the changes of atomic populations submitted to strong temperature fluctuations.     

Stark broadening of B IV lines for astrophysical and laboratory plasma research

Stark broadening parameters for 36 multiplets of B IV have been calculated using the semi-classical perturbation formalism. Obtained results have been used to investigate the regularities within spectral series and temperature dependence.     

On the Stark broadening of the Re II spectral lines

Stark broadening parameters - full widths at half maximum (FWHM) and shifts for 11 Re II lines have been calculated. The plasma parameters used were electron density of ${10}^{17}$ cm^?3 and temperature from 5 000 K to 80 000 K. Calculations were performed using the simplified modified semiempirical (SMSE) approach and compared with calculations by Cowley’s approximative Stark broadening formula at 10000 K, usefull in spectrum synthesis. The results have also been considered in the atmosphere model of A type star and for DB white dwarfs.     

Spectroscopic data and Stark broadening of Cu I and Ag I spectral lines: Selection and analysis

Optical emission and linear laser absorption spectroscopy techniques were used in investigation of plasma with copper and silver admixture. The method of selection of spectral lines and spectroscopic data with the aim of diagnostics of multicomponent air plasma with two metal vapors admixture was developed. Energy level populations behavior on the Boltzmann plot were used for Cu I and Ag I spectroscopic data selection. In this way the selection of spectroscopic data for some of Cu I and Ag I lines was realized. Stark broadening parameters of Cu I and Ag I were examined. Experimentally obtained temperature and electron density radial distributions were used in the calculation of plasma composition in the assumption of local thermodynamic equilibrium. Linear laser absorption spectroscopy was used to examine the state of plasma.     

Proton lateral broadening distribution comparisons between GRNTRN,MCNPX, and laboratory beam measurements

Recent developments in NASA’s deterministic High charge (Z) and Energy TRaNsport (HZETRN) code have included lateral broadening of primary ion beams due to small-angle multiple Coulomb scattering, and coupling of the ion-nuclear scattering interactions with energy loss and straggling. This new version of HZETRN is based on Green function methods, called GRNTRN, and is suitable for modeling transport with both space environment and laboratory boundary conditions. Multiple scattering processes are a necessary extension to GRNTRN in order to accurately model ion beam experiments, to simulate the physical and biological-effective radiation dose, and to develop new methods and strategies for light-ion radiation therapy. In this paper we compare GRNTRN simulations of proton lateral broadening distributions with beam measurements taken at Loma Linda University Proton Therapy Facility. The simulated and measured lateral broadening distributions are compared for a 250 MeV proton beam on aluminum, polyethylene, polystyrene, bone substitute, iron, and lead target materials. The GRNTRN results are also compared to simulations from the Monte Carlo MCNPX code for the same projectile-target combinations described above.     

Collisional line broadening versus collisional depolarization: Similarities and differences

Within the impact approximation, collisional line broadening parameters and depolarizing and polarization transfer (population, orientation, alignment transfer) rates are complementary: both include the effect of collisional transitions between the Zeeman sublevels of a given level, or between fine or hyperfine structure levels of a given term. However, there are several differences: in line broadening, the two levels connected by the radiative transition contribute to the broadening, and there is also an interference term between these two levels, whereas only one level or two close levels are concerned in the depolarization. Another difference lies in the fact that purely elastic collisions contribute also to the line broadening, whereas they do not contribute to the depolarization. The nature of these two kinds of coefficients are recalled. Then the possibility to find some relationships or systematic trends concerning depolarization versus collisional broadening is considered. This is to answer some current questions which come from the polarization community.     

Magnetospheric and ionospheric manifestations of interplanetary foreshocks

The geometry of a typical interplanetary shock front in the vicinity of the Earth’s orbit predicts that the leading edge of the foreshock region comes into contact with the magnetosphere a few hours ahead of geomagnetic sudden impulses (SI). There is reason to believe that the interaction of the magnetosphere with the foreshock leads to magnetic and ionospheric disturbances, which can be detected by ground-based instruments. We searched for specific precursors of SIs in data from the Scandinavian riometer network and in the short period geomagnetic pulsation data from mid-latitude magnetometers. We found that SIs were preceded by the following three features: (1) an increase in riometric absorption, (2) excitation of Pcl magnetic pulsations and (3) a spectral broadening of the Pc3 magnetic pulsations. Our observations may be useful for the study of acceleration processes in the solar wind. These observations are also of potential forecasting interest.     

太阳耀斑硬X射线高能时延和辐射展宽

本文从耀斑高能电子束流与太阳大气相互作用产生硬X射线辐射的基本事实出发,根据观测资料,提出了一个流量与能谱同步变化的注入源函数模型,研究太阳大气(靶物质)密度对耀斑硬X射线时间响应.理论计算与观测事实基本一致.主要计算结果如下:高能时延与辐射展宽是耀斑硬X射线轫致辐射时间特征的二种表现,硬X射线发射区的太阳大气密度越低,高能时延与辐射展宽效应越明显,二者之间存在显著的相关性.      

Calculating the simultaneous effect of ion dynamics and oscillating electric fields on Stark profiles

We calculate hydrogen line shapes resulting from the simultaneous Stark effect of the plasma microfield and an oscillating electric field. Like laboratory plasmas, many kinds of space plasmas are affected by oscillating electric fields with a magnitude similar to that of the microfield. Here we focus on conditions where we expect that the effect of ion dynamics and oscillating electric are both significant. The combined effect of their dynamics on the quantum emitter is retained by a computer simulation coupled to a numerical integration of the Schrödinger equation. Our calculations are applied for conditions and transitions where significant changes in the line shape allow for a diagnostic of the plasma and oscillating field.     

Line shifts observed by BCS/Yohkoh

Using the observational data of Bragg crystal spectromater on Yohkoh for the period from October, 1991 to the end of 1995, we have made a statistical study for the flares which show to be in a single loop or a single loop dominated in the SXT images. It is found that although the blue asymmetry is very common during the impulsive phase, the number of events with great total blueshift is very small. It is also found that the blueshift for most flares appears at the early impulsive phase and is temporally correlated with the broadening of the line.     

Diagnostics of hot thermal plasma in flare-associated X-ray ejections

This is the first analysis of the soft X-ray spectra of flare-associated X-ray ejections. For this aim, the Yohkoh Bragg Crystal Spectrometer data recorded before two behind-the-limb flares were selected. These flares came into view from behind the solar limb but their occurrence was preceded by an X-ray ejection which expanded faster. In consequence, for several minutes the X-ray ejection was seen alone, without the presence of the brighter flare. Parameters of the plasma obtained from a fitting of synthetic spectra to observed spectra are presented and compared to images from the Yohkoh Soft X-ray Telescope. The presence of a minor fraction of the very hot (∼30 MK) thermal plasma in X-ray ejections is confirmed. High values of the non-thermal line broadening are caused by a large extension of X-ray ejections.     

Spectral line broadening by relativistic electrons in plasmas: Collision operator

In the present work we compute the real part of the impact collision operator for the electron broadening of ion lines in plasmas, taking into account relativistic effects in the dynamics of the perturbing electron. Specifically two relativistic effects are included: The modification of the trajectory due to non-Newtonian mechanics and the modification of the velocity distribution (Maxwell–Juttner). The results are compared to the non-relativistic case.     

Fine-scale structure of solar magnetic fields

Seeing limitations of the earth's atmosphere have prevented us from spatially resolving most of the basic magnetic flux elements on the sun, since their sizes are all well below one sec of arc (excluding sunspots). No space experiment to overcome this limitation has yet been performed, but the first step will be taken with Spacelab 2.Direct mapping of the circular polarization in spectral lines provides us with information on the morphology and evolution of the partially resolved magnetic structures. In reviewing recent results, special attention is payed to the question of flux disappearance, since it is fundamental for understanding the solar cycle, and depends on a knowledge of the fine-scale structures.The strong-field (kG) nature of the photospheric flux was revealed more than a decade ago using polarization recordings in pairs of spectral lines. A breakthrough in the use of spectral information to deduce the properties of the spatially unresolved magnetic fluxtubes has recently been achieved through the conversion of a Fourier transform spectrometer (FTS) into a polarimeter for Zeeman-effect recordings. We first use the FTS data to illustrate the diagnostic contents of the line-ratio technique, and then indicate how a statistical approach with 400 Fe I lines has recently been applied. In particular we discuss the implications of the observed Stokes V asymmetries for fluxtube dynamics.Finally the ongoing search for a small-scale “turbulent” magnetic field of mixed polarities is described. Observational limits derived from direct magnetograms, spectral line broadening, and the Hanle effect are illustrated.     

Asymmetric X-ray line broadening in solar flares

The symmetry and time development of X-ray spectral lines are examined for many flares using Yohkoh Bragg Crystal Spectrometer (BCS) observations. We examine the degree of line blueshift and asymmetric broadening as a function of flare impulsiveness. The results of the analysis present a consistent observational picture for the 16 flares that were studied. The blueshift of the total flare spectrum increases with increasing fractional rate of change of flux. This result supports models that predict stronger heating in flares results in more blueshifted plasma. It also suggests that most flares will exhibit very weak or no blueshifts if the peak fractional energy release rate remains relatively low. This will be the case if stationary plasma builds up quickly by early ‘gentle’ evaporation or rapid slowing of moving plasma, even when most of the hot plasma is generated by explosive chromospheric evaporation.     

InSb光学带隙的掺杂调控研究

利用布里奇曼法进行了InAsSb半导体合金的生长,并对其结构、光学及电学特性进行了表征.研究发现,As替位掺杂造成X射线（111）衍射峰略微右移,同时其半高宽明显展宽.基于X射线衍射数据,利用Vegard定律计算出的As组分与能谱测量得到的结果基本吻合.此外,As的掺入使得材料背景载流子浓度略有上升.傅里叶变换红外光谱结果显示,As的替入使得材料带隙明显变小,拟合得到的光学带隙与通过Woolley-Warner经验公式得到的值定性一致.研究结果表明,As掺杂是减小InSb带隙,开拓其面向第二个大气窗口红外探测应用的有效途径.      

A search for the signature of microquasars in the cosmic ray iron spectrum measured by TIGER

In a recent paper Heinz and Sunyaev suggest that relativistic jets observed in microquasars might result in narrow features in the energy spectra of heavy cosmic rays with ≈1 to ≈10 GeV/nuc. They further argue that such features might be observable if there has been one or more microquasars nearby within the last few million years. We report preliminary results of a search for evidence of such features using data from a 32-day balloon flight of the Trans-Iron Galactic Element Recorder (TIGER). Although this flight took place near solar maximum, calculations of the broadening effects of solar modulation indicate that a narrow feature of sufficient intensity should still be observable. An energy spectrum for iron with high statistical significance has been derived from ≈100,000 Fe events in the energy range from about 2.5 to 10 GeV/nuc. Although our preliminary results do not reveal any obvious features, we will discuss the possibility of observing such features with TIGER and other instruments.     

The STARK-B database as a resource for “STARK” widths and shifts data: State of advancement and program of development

“Stark” broadening theories and calculations have been extensively developed for about 50 years and can now be applied to many needs, especially for accurate spectroscopic diagnostics and modeling. This requires the knowledge of numerous collisional line profiles. Nowadays, the access to such data via an online database becomes essential. STARK-B is a collaborative project between the Astronomical Observatory of Belgrade and the Laboratoire d’Étude du Rayonnement et de la matière en Astrophysique (LERMA). It is a database of calculated widths and shifts of isolated lines of atoms and ions due to electron and ion collisions (impacts). It is devoted to modeling and spectroscopic diagnostics of stellar atmospheres and envelopes, laboratory plasmas, laser equipments and technological plasmas. Hence, the domain of temperatures and densities covered by the tables is wide and depends on the ionization degree of the considered ion. STARK-B has been fully opened since September 2008 and is in free access.     

Thermospheric winds over Abuja during solar minimum period

Monthly variations of averaged nighttime thermospheric winds have been investigated over Abuja, Nigeria (Geographic: 9.06°N, 7.5°E; Geomagnetic: 1.60°S). The reports are based on Fabry-Perot interferometer measurements of Doppler shifts and Doppler broadening of the 630.0 nm spectral emission. The results were obtained during a period of weak solar activity with the solar flux (F10.7) typically below 70 solar flux units. Inspection of the average monthly thermospheric winds from October 2017 to December 2017 found December meridional winds to be more equatorward than the October and November winds. Zonal winds are eastward with pre-midnight maximum speeds going above 100 m/s. Compared to Jicamarca zonal winds in the Peruvian sector for the same month of October, the magnitude of maximum Abuja zonal wind speed is weaker. We compare the observed diurnal variation with the recently updated Horizontal wind model (HWM 14). Most of the observational features of thermospheric wind diurnal variation are captured in the model variation. The HWM14 generally showed good agreement with the Abuja October and November zonal wind observations but overestimates the December meridional winds. Expected longer period analysis of the results from Abuja will stimulate a better understanding of wind climatology over the West African sector.