Gravity anomaly during the Mohe total solar eclipse

By using a high-precision LaCoste-Romberg (D-122#) gravimeter, continuous and precise measurements were carried out during the March 9, 1997 total solar eclipse in the Mohe region in Northeast China. The gravity variations were digitally recorded during the total solar eclipse so as to investigate the possible anomaly of the sun and the moon’s gravitational fields on the earth. After the careful processing and analysis of the observed data, no significant anomaly during the very solar eclipse has been found. However, there are two ‘gravity anomaly valleys’ with near symmetrical decrease of about 6–7 μGal at the first contact and the last contact. This is the anomaly phenomenon observed and reported for the first time in the literature. This note presents some analyses and discussions.     

水滑坡体产生的涌浪特性

入水滑坡体所产生涌浪的波峰高度及传播时间是此类灾害预警和风险评估最为关注的特性参数。本文通过对滑坡体和水波相互作用的耦合数学模型进行数值求解,研究了以上2个特性参数与滑坡体形状及运动过程的关系。数学模型中假设滑坡体兴波区域内水波横向能量扩散可忽略,在立面二维的简化下应用非线性浅水方程描述水波过程;假设滑坡体底部流体法向流速为零,应用简化的Novier-Stokes方程描述底部流动;在滑坡体的运动方程中考虑了惯性力、水波波动压力、底部流体对滑坡体的阻力和浮托力以及滑坡体和滑动面间的摩擦力等。数值结果表明:滑坡体水平速度越大,涌浪传播越快;当滑坡体水平速度接近波速时,滑坡体具体形状对波峰高度有显著影响;当滑坡体水平速度大于波速时,波峰高度随滑坡体速度的增大而减小。因此,以往数学模型中对滑坡体具体形状的忽视,或者设定过大的滑坡体速度,都有可能导致波峰高度的低估,不利于防灾减灾。     

日月食限的计算

日月食的观测对太阳物理学、天文学及其它相关学科的研究有重要意义．然而准确的日月食预报却离不开日月食限的计算．本文研究了日月食计算方法，力求简单易懂，以便于课堂教学和进行科普教育．     

Ionospheric responses to a total solar eclipse deduced by the GPS beacon observations

The total electron content (TEC) data during the total eclipse of March 9, 1997 were collected, which were observed by means of nine GPS receivers located at the eastern Asia. The responses of total TEC to the eclipse were analyzed. The results show that: 1) the eclipse led to apparent decrement in TEC that lasted for six to eight hours; 2) the maximum decrement occurred after the middle of the eclipse with time-delays varying from twenty minutes to about three hours; 3) the maximum absolute deviations of TEC on the eclipse day do not show a simple and consistent relationship to the maximum solar obscuration. Foundation item: Supported by the National Natural Science Foundation of China(49684002) Biography: CHEN An-hua (1976-), female, Master candidate. Research interests: studying ionosphere by GPS beacons.     

日月食观测在科学研究上的意义

阐述了日月食观测在研究太阳大气结构、太阳活动，寻找近日彗星和水内行星，检验广义相对论理论以及校正历史中年日次序诸多方面的价值．     

海浪感应磁场的频谱特性

根据Maxwell电磁理论,在地磁场中运动的海水将产生磁场。从理论上计算出海浪在地磁场中感应磁场的频谱是一种窄带频谱,随着海水深度的增加或风速的增加,其频带宽度变窄、峰值频率向低频方向移动。     

Tomographic Study of Ionospheric Effects Associated with a Solar Eclipse

This paper studies the ionospheric effects associated with the solar eclipse of October 24th, 1995 by means of Computerized Ionospheric Tomography (CIT). Since the reconstructed profiles from experimental CIT are sporadically located in time, a time domain interpolation method based on Singular Value Decomposition (SVD) technique is proposed and applied to extract the ionospheric effects. The effects can be extracted by comparison analysis between the interpolated CIT profiles of the eclipse days and that of the reference day that are time-aligned. A series of figs have been obtained showing the attenuation of photonization effect at low altitudes and the weakening of plasma's transportation process at high altitudes, etc. The photonization effect recovered to normal level soon after the last contact. The maximum electron density diminishing is observed about 2 h after the eclipse maximum and the effects seem vanished in the hours followed. Analysis on vertical TEC's latitudinal-temporal variation gives     

《明天历》日食算法分析

目的用数学公式将《明天历》的日食算法表达出来,并指出其天文学意义。方法文献分析与数学建模。结果《明天历》先求得合朔时交点离开冬至点的距离以及太阳到冬至点的距离,两者的差值就是"去交度分";常数中的"朔差"是一个朔望月中交点退行的距离;它以恒星年而不以回归年入算以及用太阳的去交分代替月亮的去交分都是其去交度分算法的不足之处。《明天历》的食甚时刻仅是对经朔时刻加入日月不均匀运动有关的修正,没有进行时差的修正。其他算法与主流算法基本相同。结论《明天历》的日食算法在宋代是比较特殊的,这些特殊之处大部分是正确的、合理的,但某些算法中仍存在不足。     

Recent progress in solar physics made during the program of 2008 August 1st solar total eclipse

The development of solar physics is presented from the program of 2008 total eclipse in China, including the presentations in the international workshop in this period and some observational results of the solar eclipse.     

Rossby waves on the Sun as revealed by solar 'hills'

It is a long-standing puzzle that the Sun's photosphere--its visible surface--rotates differentially, with the equatorial regions rotating faster than the poles. It has been suggested that waves analogous to terrestrial Rossby waves, and known as r-mode oscillations, could explain the Sun's differential rotation: Rossby waves are seen in the oceans as large-scale (hundreds of kilometres) variations of sea-surface height (5-cm-high waves), which propagate slowly either east or west (they could take tens of years to cross the Pacific Ocean). Calculations show that the solar r-mode oscillations have properties that should be strongly constrained by differential rotation. Here we report the detection of 100-m-high 'hills' in the photosphere, spaced uniformly over the Sun's surface with a spacing of (8.7 +/- 0.6) x 10(4) km. If convection under the photosphere is organized by the r-modes, the observed corrugated photosphere is a probable surface manifestation of these solar oscillations.     

Rocket UV flash spectra from the solar eclipse of March 7, 1970

Flash spectra of the total solar eclipse throughout all its phases have been obtained in the extreme ultraviolet for the first time.     

Drag increment due to internal waves generated by Rankine ovoid

The experimental results on drag increment caused by internal waves, which are generated by a Rankine ovoid towed horizontally at constant velocities in a two-layer stratified water (a strong pycnocline) initially at rest, are presented. The drag increment due to stratification is obtained experimentally as a function of internal Froude number Frd and Reynolds number Re. From the results, it is shown that as a function of Frd or Re, an increment in mean drag coefficient due to stratification ΔCd has both increasing and decreasing region attributable respectively to internal wave and to collapse of mixing fluids in the wakes. A most significant result shows that when Frd=0.838 there exists a maximum of ΔCd, which is equal to 0.05 in the exciting region of the strong internal wave generation.     

涡旋波干涉振幅全息图的计算机制作

根据数学模型,借助计算机语言编程制作了涡旋波干涉的振幅全息图.结果表明:涡旋波分别与平面波和球面波干涉,形成叉形光栅和螺旋环形光栅全息图样,且图样分布随涡旋波拓扑荷值的变化而变化.当拓扑荷值由正整数变为负整数时,叉形光栅的开口方向和螺旋环的旋转方向发生反转;当拓扑荷值变为分数时,全息图样发生不同程度的位错.该全息图可作为振幅掩模或直接加载于液晶空间调制器,用于生成涡旋光束.