Formation of a filamentary structure in planetary nebulae

Intricate filamentary structure and multiple shell-like appearance are very common phenomena in Planetary Nebulae.In addition, recent observations also indicate that the individual filaments present in these objects can have larger velocities than the adjacent smooth background (Pascoli, 1992 PASP 104, 350 and paper quoted therein).We have hypothesized that non linear hydrodynamical processes existing within the nebular gas are, possibly, responsible for these structures. As a matter of fact, it is argued that such a characteristic morphology, reinterpreted as a intermingled network of solitary waves or solitons, can be spontaneously generated in Planetary Nebulae as soon as one assumes that the nebular gas is permeated by a weak magnetic field whose strength is about 10^–5 to 10^–4 gauss.Main results of this work and further comments will be subsequently published in Ap&SS.     

Eclipse observations of coronal emission lines. I. [Fex] 6374Å profiles at the eclipse of 16 February 1980

Coronal spectra during the total solar eclipse of 1980 February 16, were obtained in the 6374Å [Fex] line using a multislit spectrograph. These spectra have a dispersion of 2.5 Å mm^-1. The observed line profiles from 1.1 to 1.7 R_⊙ with a spatial resolution of 10 × 22 arcsec², give half-widths that vary between 0.6 Å and 2.4Å. A large number of locations have half-widths around 1.3 Å corresponding to a temperature of 4.6 × 10⁶ K. If temperature of the order of 1.3 × 10⁶ K are typical of the regions that emit [Fex], then turbulent velocities of ~ 30 km s^-1 need to be invoked for the enhanced line broadening. The line-of-sight velocities measured range between +14 km s^-1 to -17 km s^-1. Most of the locations have velocities less than ±5 km s^-1. From these observations we conclude that corona does not show any localized differential mass motion and that it co-rotates with the photospheric layers deeper down.     

试谈太阳能供电系统充电控制器的改进

叙述了山西大同数字遥测地震台网建设过程中，对镇川台太阳能供电系统进行改进的情况，讨论了在地震观测系统中使用太阳能供电系统应考虑的问题，提出了相应的解决办法。指出，根据地域、气候等条件合理设计太阳能电池的容量，合理设置控制器的浮充电流，可使太阳能电源系统处于较佳的工作状态。     

日本古代的一次可能的日全食与地球自转变化

利用古代日食观测记载研究地球自转长期变化的方法和已有的结果为基础，研究了日本的古书中记载的可能与古代一次日全食有关的“天门”传说，及朝鲜的古书中与此有关的记载。本文的结果支持一些学者认为这个传说是由发生于公元158年7月13日的日全食引起的观点，并在历书时ET系统下计算分析了该日食的参数，由此得到表示地球自转变化的△T值约为2．22小时。     

太阳风引起的地磁场扰动的系统辨识

本文利用最小二乘非参数辨识,在线性时不变假设下,对由太阳风变化引起的地磁场扰动进行了研究.用这种方法得到的脉冲响应函数给出了地磁层对太阳风变化响应的宏观外部描述,同时还得到了较好的地磁扰动预报结果.本文不仅对单输入单输出系统（SISO系统）进行了分析,而且也对多输入单输出系统（MISO系统）进行了讨论.     

100—200km热层大气光电离率及电子密度剖面对太阳活动的响应

本文利用新的太阳EUV辐射资料、中性大气结构模式及大气成分的吸收及电离特性,计算了100—200km大气的光电离率随高度、太阳天顶角及太阳活动的变化,求得了E-F_1谷的变化特征;利用完整的光化模式求得了电子密度随太阳天顶角的变化及对太阳活动的响应,并与IRI模式作了比较.结果表明,1.太阳活动指数与光电离率间的相关关系一般为正,但在一定的高度范围内,或在天顶角大于临界值X_(cr)=60°时,两者之间可出现负相关;2.太阳活动明显地影响E-F_1谷高与谷厚,当天顶角不变时,谷高与谷厚均与太阳活动成正相关;3.本模式与IRI间的偏差因子明显随高度及太阳天顶角而变化.     

太阳风引起的地磁扰动的参数辨识

作为太阳风引起的地磁扰动的系统辨识一文的姊妹篇,本文利用参数系统辨识方法,对太阳风-磁层耦合系统做了进一步的探讨.根据地磁扰动机制的理论研究,地磁扰动被认为是太阳风能量耦合进入磁层以及由此引起的一系列磁层内能量的输运和耗散的结果.在此基础上,对太阳风-磁层系统的非线性情况进行了讨论,建立了D_st指数与太阳风参量的非线性函数关系,给出了由此得到的地磁扰动计算结果.同时还利用1967年2月3-12日和1980年12月16-23日的两次事件,对已得到的函数关系进行了验证和讨论.验证结果不仅对模型的合理性、普适性做了很好的说明,也表明这种非线性函数关系作为定量的地磁预报模型,具有一定的可信度和实用性.     

太阳风能量向赤道电离层的传输

从太阳风和地磁参数综合分析出发，将研究太阳风能量输运的范围扩展到了赤道电离层区．同时也对Ａｋａｓｏｆｕ的能量耦合函数作了检验．传输到中低纬电离层的太阳风能量约为极光区焦耳加热能耗的１／１０．能量耦合的赤道电集流效应（包括电动耦合和动力耦合两部分）是十分明显的．     

Measurements of chemically and biologically effective radiation reaching the ground

Solar ultraviolet radiation at the surface has been measured at Potsdam on cloudless days by spectrometer OL 752/10. The measurements are compared with broad-band filter measurements and with model calculations using a modified version of Green's model, which is independent of the measurements. Input data to the model such as atmospheric ozone and aerosol optical thicknesses were measured by a Dobson and Brewer spectrophotometer as well as a Linke Feussner pyrheliometer, respectively. Differences between the model and the measurements are discussed in terms of uncertainties in the calibration and errors of instruments as well as uncertainties in the model calculations including the errors of input data. It is demonstrated that different chemically and biologically effective radiances can be determined from only one set of measured spectral irradiance components, i.e. global radiation and diffuse downward and upward directed radiation. Examples of diurnal variations of the photochemical production of ozone and hydroxyl radicals as determined from spectral irradiance measurements and measured concentrations of relevant trace gases are given.It is shown from the measured irradiance that relations between different effects of radiation to the biosphere depend on solar zenith angle, and to a certain extent also on atmospheric ozone. This has to be taken into account when adverse effects of changing UV radiation are evaluated. Radiation Amplification Factors derived from measurements correspond to those determined from model calculations.     

太阳散射辐射的分光测量及其能量分配

近十余年来，国内外不少学者先后研究了散射辐射与总辐射的关系［１－６］，建立了各种计算散射辐射的经验公式，但有关分光散射辐射分量的测量和研究为数甚少。为此，我们于１９８９－１９９０年在北京对３００－２８００ｎｍ光谱范围内的７个波段的散射分量进行测量，并研究了各分量与全谱段散射总量间的定量关系。