Large turbulent elements in supergiant photospheres

During the cool phase of the super-supergiant HR 8752, which happened around 1973, when the star's spectral type was K2...K5 Ia⁺, the most probable vertical extent of the main turbulent elements in the star's photosphere was about 6 times the density scale height, which is about half the stellar radius. In early-type photospheres (class Ia) it is about 10 times the atmospheric density scale height (about 0.25 of the stellar radius), while in less extreme (luminosity class Ib) medium-type supergiants the most probable vertical extent of the elements is approx. 8 times the density scale height (0.05R). Large turbulent elements are apparently a common feature in supergiant photospheres; the more extreme the supergiant the larger the relative size of the eddies.     

Heating of the solar transition zone and corona

Theoretical temperature, velocity and density profiles for the area above an optical depth = 10^–8 in the Sun were computed. An approximation for the coefficient of thermal conductivity was used; dissipation of shock wave energy as well as that of sound wave energy was taken into account and the height of shock formation was determined by a condition on the pressure. Comparison shows that our theoretical curves correspond very well with the observations.     

Evolution of massive close binaries

The evolution of a binary system with components of 10M and 8M is computed through a case B of mass exchange. It is found that after the end of core helium burning, a second stage of mass transfer from the primary occurs. Carbon ignition is prohibited by the large neutrino losses in the degenerated core. The primary remnant, a 1.12M star, ends as a white dwarf. A comparison with the 10M single evolution is made.This research is supported by the National Foundation of Collective Fundamental Research of Belgium (F.K.F.O.) under No. 10303.     

The spectrum of Cyg X-1 — A theoretical model

We have calculated the spectrum of Cyg X-1 under the assumption that the radiation orginates in a disk around a 11M black-hole. Supersonic turbulence prevails in the outer parts of the disk and electron-electron bremsstrahlung appears to be resonsible for the maintenance of the temperature at a level less than 10¹⁰ K near the inner edge of the disk. The theoretical spectrum gives the best fit with the observations if the Reynolds number is about 1200.     

电子政务中的人口空间管理和分析

介绍了在国家级人口地理信息系统中 ,利用 2 0 0 0年人口普查信息 ,采用三维模型显示、罗伦斯曲线、人口重心和人口潜力等方法 ,宏观分析了中国人口分布的特征。并在城市人口地理信息系统的基础上 ,通过对城市零售单位布局的分析 ,介绍了人口地理信息系统的微观分析和应用过程     

四合屯-义县地区义县组火山活动的旋回性特征

在岩石学特征分析的基础上,结合本区广为发育的火山间歇期沉凝灰岩、凝灰质粉砂岩以及其中的古生物化石特征等,作者将四合屯-义县地区义县组火山活动分为早、中、晚3个火山活动旋回,即早期以玄武岩、玄武安山质火山岩类为主的基性、中基性旋回;中期以流纹质及英安质火山岩类为主的中酸性旋回;晚期以玄武岩为主的基性旋回.义县组火山活动早期的基性、中基性旋回还可进一步分为4个亚旋回,在其中的沉凝灰岩中发育有以鹦鹉嘴龙为主的古脊椎动物化石.各旋回或亚旋回的底部不同程度地发育有爆发-沉积相的沉凝灰岩或内陆湖泊相沉积岩.包括珍稀动植物在内的热河生物群化石则产于义县组火山活动中期的沉凝灰岩以及钙质页岩之中.     

砂岩型铀矿床地浸地质工艺性能综合定量评价指标--地浸指数的设计与应用

从砂岩型铀矿床地浸开发工艺着手，通过对其地质影响因素分析，结合各因素对地浸开发的影响程度，提出了砂岩型铀矿床地浸的地质工艺性能综合评价指标——地浸指数(LI)，并建立了其计算模型。通过计算地浸指数可定量地了解待开发矿床或块段的地浸开发适宜程度。地浸指数LI值越大，说明该矿床地浸的地质工艺性能越佳、越有利于地浸开发。通过对伊犁盆地512模型铀矿床、511铀矿床及吐哈盆地十红滩铀矿床的LI值试算，得到的LI值分别为119．95、102．56和47．8l。试算结果表明，511矿床很有利于地浸开发，511矿床地浸开发的有利性逊于512矿床，十红滩矿床属于不利于地浸的范畴，建议放弃酸法地浸方案，寻求低酸法地浸、清水地浸或减法地浸等方案。结合3个矿床的工业开发实际和前期试验成果，初步确定砂岩型铀矿床地浸地质工艺性能的LI值区间：LI≥100，很有利于地浸；80≤LI＜100，有利于地浸：LI＜80，不利于地浸。     

中国煤和烃源岩镜质组的激光诱导荧光显微特征及其应用

应用自行组装的激光诱导荧光显微光度计(LIFM)系统地研究了中国煤和烃源岩中镜质组的荧光强度及荧光变化，建立了镜质组的荧光变化与成熟度之间的相关模式图(R-I-VRo)，该图可解决镜质组反射率抑制问题，并将烃源岩成熟度评价范围扩展到VRo达2．0％左右，该方法对于正确评价烃源岩成熟度具有广泛的应用前景。