Multi-wavelength Diagnostics of Bombardment by Non-thermal Particles in Solar Flares

Chromospheric lines, including Ha, Lyα, Lyβand CaⅡK, CaⅡ8542, are systemically and quantitatively investigated with respect to the non-thermal excitation and ionization due to particle beam bombardment for a series of solar semi-empirical atmospheric models. As a result we propose to use the contrast in the integrated intensity of hydrogen lines to estimate the total energy flux of the bombarding beam during the solar flare impulsive phase. Partial frequency redistribution is considered in the Lyαline calculation and a smaller intensity enhancement in the Ha line-centers is found than in the previous results of Fang et al.     

汞型活性炭纸富集-XRFA法测定水样中的痕量SCN^-

SCN^-的测定大都采用分光光度法[1，2]。用波长色散X-射线荧光光谱测定痕量SCN^-的方法，至今尚未见报道。     

A New Solar Radio Spectrometer at 1.10-2.06 GHz and First Observational Results

An improved Solar Radio Spectrometer working at 1.10-2.06 GHz with much improved spectral and temporal resolution, has been accomplished by the National Astronomical Observatories and Hebei Semiconductor Research Institute, based on an old spectrometer at 1-2 GHz. The new spectrometer has a spectral resolution of 4 MHz and a temporal resolution of 5ms, with an instantaneous detectable range from 0.02 to 10 times of the quiet Sun flux. It can measure both left and right circular polarization with an accuracy of 10% in degree of polarization. Some results of preliminary observations that could not be recorded by the old spectrometer at 1-2 GHz are presented.     

关于波浪Boussinesq方程的研究

对有关波浪 Boussinesq方程的研究成果进行了系统的归纳总结和评述 ,以期对本学科的发展起到一定的引导和促进作用     

迭代折射静校正技术在鄂北地震资料处理中的应用

在低速层速度(地表直达波)已知的条件下,利用生产炮初至信息,用加权最小平方法和共轭梯度法建立的折射静校正数学模型,迭代求取长波长、短波长静校正量,在解决鄂尔多斯盆地北部的虚假小幅度构造问题及改善剖面质量方面取得了明显的效果。     

低共结系统中不同几何类型振荡分带的成因动力学解释

低共结系统中存在着两种固溶体交替结晶生长和同时耦合结晶生长这两种生长方式，当液相组分的扩散慢时有利于共晶的交替结晶生长，液相组分的扩散快时有利于共晶的耦合生长。前看有利于形成具有宏观振荡波长球（环）状或条带状分带，后者有利于形成细观振荡波长的层状构造。不规则的周期分带现象与内部非线性机制和外部扰动因素有关。     

紫外辐射如何影响人类

太阳辐射能量的波长范围较宽，对人类而言，其中大部分的太阳辐射是肉眼无法看得见的。波长越短，辐射强度越大，并且对于生物体潜在的危害也就越大。到达地球表面的紫外辐射，其波长在290～400nm(十亿分之一米)，这比可见光的波     

读诗谈天象之五 大气造成的天文现象(下)

大气折射对天文观测的影响大气折射还造成另一个影响天文观测的效应,称为大气色散。原来,空气的折射率还与光的波长(即颜色)有关,不同颜色的光在相同的介质中传播,因折射率不同而分散,雨后彩虹展现由红到紫的七色景象,正是由于同样原因(光被悬浮在空气中的小水滴折射并产生色散)。由于大气色散,使得我们观测到的天体像,无论是目视的眼睛所见还是照相的底片留影,星像都呈现为一条垂直的细小光谱,紫端靠近天顶。天顶距越大,色散也越大。