太阳大气中湍动场对CaⅡK线的影响

本文运用黑子半影模型研究了中介湍动场对太阳大气中CaII K线的影响。结果表明,空间分辨率的提高以及湍动元长度的增加均可导致观测谱线轮廓的不对称。当湍动元长度小于40km时,中介湍动场可以用微观和宏观湍动的组合来模拟,对大气模型及谱线轮廓的计算基本无影响;但当湍动元长度大于40km时,这种简化的处理方法可能导致大气模型上层色球温度偏高。文中通过一个计算实例,说明了在太阳大气模型计算中,只用中介湍动也可能使谱线的理论轮廓同观测基本相符。      

武汉中层、低热层大气角谱中频雷达观测

武汉中频雷达是利用中层、低热层中电子密度不均匀体的散射来测量大气的水平风场和电子密度剖面。雷达在计算风场的过程中可得到一些该层大气中电子密度不均匀体的寿命和空间尺度等参量值。结合这些参量和大气风场值可计算得到大气的角谱。其计算方法包括全相关分析技术的谱宽法和空间相关法。前者计算的值被认为是大气角谱的上限值。应用这两种方法,利用2001年2月9日武汉中频雷达的观测数据,对武昌上空中层、低热层大气的角谱进行了计算。结果得到大气角谱随高度增加略微增加,如在68km为6°,90km达最大为11°,其平均值为9.2°。利用2001年2月4—10日86km高度上的数据,得到一个7天平均的日变化曲线,发现大气角谱值在本地夜晚最小。     

航空发动机机匣损伤容限评估及剩余寿命预测

使用有限元的方法,建立了某航空发动机机匣安装座处局部模型,计算得到了不同尺寸裂纹的应力强度因子的形状因子Y.基于BS7910评定方法,利用失效评估图(FAD,Failure Assessment Diagram)确定了机匣安装座结构在工作应力下的可接受裂纹尺寸为84.8 mm,结构的剩余强度随裂纹尺寸的增加而显著降低,焊缝较母材具有更低的损伤容限和剩余强度.使用缩小宽度模拟验证件模拟工作状态载荷进行了验证试验,当裂纹尺寸与试样宽度比值较小时,与模拟验证件的评估结果基本吻合.根据Paris公式,构件在工作应力下的剩余寿命为74 238周次.      

极区F层不规则结构的分形模型

本文利用1986年9—12月期间17个电离层吸收事件的Riometer资料计算了电离层闪烁强度的Fourier谱和Bessel谱。求出了谱遵从的k~(-β)型函数的β值,1.8<β<2.5,平均为2.1;求出了不规则结构的漂移速度平均为129m/s。计算了各个事件的闪烁指数S_4<0.4。求出相位涨落空间谱,且指出其也遵从幂型函数k~(-α)规律。根据上述结果,本文提出极区F层不规则结构为分立的分形,不是分立的“斑块”。利用β值求出分形的分数维D=2.45。给出了不规则结构的近似分形模型。     

一种全球临近空间大气密度建模方法及应用

基于TIMED/SABER卫星2002—2018年观测的20~100 km大气密度数据，统计获得多年月平均值和标准偏差的全球网格数据。利用网格数据，分析了大气密度的变化特征。以网格数据为基准，计算了USSA76的相对偏差，分析了USSA76相对偏差的分布特征。以网格数据为驱动，将大气密度表征为平均值与大尺度扰动量和小尺度扰动量的加和，大尺度扰动和小尺度扰动分别采用余弦函数和一阶自回归模型表征，初步建立了全球临近空间大气密度模型。通过对比模型仿真值与激光雷达观测值，表明模型仿真值与观测值具有较好的吻合度，验证了建模方法的可行性。利用蒙特卡罗方法可再现给定轨迹上所有可能的大气状态。      

重力波对中间层和低热层大气环流的影响

利用β通道准地转近似大气平均运动方程组,采用重力波线性饱和参量化方法,定性地研究大气重力 波对中间层和低热层大气环流的作用.模拟计算得到,大气重力波对平均东西风速可产生100m·s-1／d左右的作 用力和产生120 m2/s的湍流扩散,这些作用平衡了Coriolis扭力,导致大气的平均东西风速大大偏离辐射平衡 风场,中层顶附近的平均东西风速在冬季(夏季)甚至反转为东风(西风).平均东西风速计算结果与冬季和夏季 中频雷达东西风速观测值和大气模式剖面等大致一致.     

Be／X射线双星LSI＋61°303的光谱研究

给出了１９９２－１９９５年Ｂｅ／Ｘ射线双星ＬＳＩ＋６１°３０３每年的光谱观测结果，分析了光谱发射线轮廓及其变化，观测显示Ｈβ发射线轮廓具有典型的气壳吸收，表明观测视线与Ｂｅ星赤道平面平行，同时发现Ｈα发射线参数发等值宽度和双峰强度之比也具有类似射电流量的周期性变化，但其变化与射电玫光学光度的变化不同，因此认为此变化可能与中子星周期的吸积盘及其轨道交食有关。     

一种测量激光束光斑尺寸的方法

给出了一种测量激光束光斑尺寸的简单方法。在本方法中，当激光束光斑横向扫过一个直边界时，边界衍射波的强度轮廓曲线就可观测得到。从强度轮廓曲线可测量光斑尺寸。一束氦氖激光的光斑尺寸经测量为８．３μｍ，用刀口法测得该值为８．９μｍ。     

Observational astrochemistry: recent results.

More than 80 molecular species have now been observed by astronomers in the dense interstellar clouds where stars and planets form or in the envelopes expelled by evolved stars. Elemental constituents of these compounds include all of the "biogenic" elements, hydrogen, carbon, nitrogen, oxygen, sulfur, and (most recently) phosphorus. In addition, silicon is found in several molecules, and a series of metal halides have recently been detected in the outflowing envelope of a nearby carbon star. Additions to the list of known interstellar molecules since the last COSPAR meeting are discussed individually. Recent measurements of the hydrogen isotopic fractionation for the cyclic molecule C3H2 are described; values up to 10,000 times the cosmic deuterium-to-hydrogen ratio are found. Knowledge of the chemical reservoirs for the major volatile elements and a comparison between observed molecular abundances and theoretical models are both discussed.     

A statistical study of C IV regions in 20 Oe-stars

In this paper, using the Gauss-Rotation model (GR model), we analyse the UV C IV resonance lines in the spectra of 20 Oe-stars of different spectral subtypes, in order to detect the structure of C IV region. We study the presence and behavior of absorption clouds and analyse their characteristics. From this analysis we can calculate the values of a group of physical parameters, such as the apparent rotational and radial velocities, the random velocities of the thermal motions of the ions, the Full Width at Half Maximum (FWHM), the optical depth, as well as the absorbed energy and the column density of the independent regions of matter, which produce the main and the satellite clouds of the studied spectral lines. Finally, we present the relations between these physical parameters and the spectral subtypes of the studied stars and we give our results about the structure of the C IV region in their atmosphere.     

The structure of the solar corona as observed by the Solar Extreme ultraviolet Rocket Telescope and Spectrograph

Data from the Solar Extreme-ultraviolet Rocket Telescope and Spectrograph (SERTS) have been used to address a number of important scientific problems. The primary strength of the SERTS data is the fact that this spectral range is rich with emission lines. Over 270 lines are seen in the SERTS active Sun spectrum, from 57 different ions. For example, multiple (≥4) lines are observed for all ionization states of iron from Fe IX to Fe XVII. Temperatures and densities have been derived for a number of active and quiet Sun regions, the coronal magnetic field strength has been estimated for both a plage region and an active region.     

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.     

Cosmic ray H/H ratio measured from BESS in 2000 during solar maximum

The Balloon-borne Experiment with a Superconducting Spectrometer (BESS) was flown from Lynn Lake, Manitoba, Canada in August, 2000, during the maximum solar modulation period, with an average residual atmospheric overburden of 4.3 g/cm². Precise spectral measurements of cosmic ray hydrogen isotopes from 0.178 GeV/n to 1.334 GeV/n were made during the 28.7 h of flight. This paper presents the measured energy spectra and their ratio, ²H/¹H. The results are also compared with previous measurements and theoretical predictions.     

Validation of satellite-derived atmospheric temperature and water vapor concentration using radiosonde and rocketsonde measurements

Measurements of the spectral radiance of the earth's atmosphere from satellites can be related to the vertical structures of temperature and humidity. Derived profiles of these quantities are compared with radiosonde and rocketsonde observations, as well as with horizontal and vertical cross-sections of the atmosphere. In some regions of the atmosphere, particularly where large gradients are found, significant differences occur. A method for overcoming these by use of Typical Shape Functions is discussed. Transmittances computed from theory require modifications which are not well defined, and radiances measured from some satellite instruments disagree with computed values in ways which suggest calibration or instrument problems.     

Spectroscopy peculiarities of thermal plasma of electric arc discharge between electrodes with Zn admixtures

Plasma of the free burning electric arc between Ag–SnO₂–ZnO composite electrodes as well as brass electrodes were investigated. The plasma temperature distributions were obtained by Boltzmann plot method involving Cu I, Ag I or Zn I spectral line emissions. The electron density distributions were obtained from the width and from absolute intensity of spectral lines. The laser absorption spectroscopy was used for measurement of copper atom concentration in plasma. Plasma equilibrium composition was calculated using two independent groups of experimental values (temperature and copper atom concentration, temperature and electron density). It was found that plasma of the free burning electric arc between brass electrodes is in local thermodynamical equilibrium. The experimental verification of the spectroscopic data of Zn I spectral lines was carried out.     

Near infrared studies of the massive X-ray binary 2S 0114+65

We present near-infrared spectroscopy of the massive X-ray binary 2S 0114+650. These observations covering the spectral range 1.08–2.35 μm span the region where Paschen and Brackett series recombination lines of hydrogen are expected to be seen, namely, Paβ , Brγ and Br 10–17 lines. The absence of any of these lines in emission supports earlier inferences that the optical component in 2S 0114+650 is unlikely to be a Be star but rather a B type supergiant. Near-IR photometry gives J = 8.78, H = 8.53 and K = 7.96; these values show marginal variations from earlier reported measurements.     

The CO2 greenhouse effect and the thermal history of the atmosphere.

The influence of the expected rise of CO2 content in our atmosphere upon terrestrial temperature is uncertain. A significant increase in temperature could be threatening to certain aspects of terrestrial biology. On the other hand, it is a general consensus among paleobiologists that the Earth possessed a CO2 atmosphere in the past billion years, without dramatic temperature variations endangering the continuity of life. In order to clarify this problem, and to contribute to the understanding of the CO2 greenhouse effect on Venus we have computed the absorption spectrum of CO2 for a wide range of atmospheric concentrations. More than 2500 spectral lines of the 15 micron band were taken into account in our line-by-line calculation. We have used an empirical exponential line-shape function at the line edges. Our results agree with the experimental data of F. W. Taylor. The estimated increase in surface temperature does not reach the boiling point of water even for CO2 concentrations thousands of times larger than the present concentrations. Higher energy (>666 cm-1) CO2 bands and/or an increase in atmospheric H2O may, however, amplify the greenhouse effect.