Ionospheric measurements of relative coronal brightness during the total solar eclipses of 11 August, 1999 and 9 July, 1945

Swept-frequency (1/10 MHz) ionosonde measurements were made at Helston, Cornwall (50°06N, 5°18W) during the total solar eclipse on August 11, 1999. Soundings were made every three minutes. We present a method for estimating the percentage of the ionising solar radiation which remains unobscured at any time during the eclipse by comparing the variation of the ionospheric E-layer with the behaviour of the layer during a control day. Application to the ionosonde date for 11 August, 1999, shows that the flux of solar ionising radiation fell to a minimum of 25±2% of the value before and after the eclipse. For comparison, the same technique was also applied to measurements made during the total solar eclipse of 9 July, 1945, at Sörmjöle (63°68N, 20°20E) and yielded a corresponding minimum of 16 ± 2%. Therefore the method can detect variations in the fraction of solar emissions that originate from the unobscured corona and chromosphere. We discuss the differences between these two eclipses in terms of the nature of the eclipse, short-term fluctuations, the sunspot cycle and the recently-discovered long-term change in the coronal magnetic field.     

几种静校正方法的比较研究

为解决近地表速度异常和地形起伏引起的静校正问题,已出现了多种静校正方法,这常常使资料处理人员无所适从。这里从众多的静校正方法中选择了三个具有代表性的,在生产中用得较多的方法(折射静校正、无射线追踪层析静校正、非线性层析静校正),从方法原理、方法特点、实际应用效果等方面进行了比较研究,最后给出了针对不同目标选择适当静校正方法的建议,以帮助资料处理人员在实际资料处理中,有针对性地选择静校正方法,快速有效地完成资料处理任务,提高处理质量。     

多项式的井间地震速度场反演方法

基于契比雪夫多项式的旅行时反演方法,不需进行入射角扫描,首先用多项式表示出深度和慢度,计算出从源点到接收点的旅行时间,通过与实际时间的误差修改模型参数,经过反复迭代,最终得到地下复杂构造的界面形态和速度变化。与网格化速度反演方法相比,计算的未知数少,对初始地质模型的依赖性小。模型试算表明,在初始地质模型与实际地质模型差别较大时,仍能取得比较好的反演结果。     

Atmospheric Electrification in the Solar System

Atmospheric electrification is not a purely terrestrial phenomenon: all Solar System planetary atmospheres become slightly electrified by cosmic ray ionisation. There is evidence for lightning on Jupiter, Saturn, Uranus and Neptune, and it is possible on Mars, Venus and Titan. Controversy surrounds the role of atmospheric electricity in physical climate processes on Earth; here, a comparative approach is employed to review the role of electrification in the atmospheres of other planets and their moons. This paper reviews the theory, and, where available, measurements, of planetary atmospheric electricity which is taken to include ion production and ion–aerosol interactions. The conditions necessary for a planetary atmospheric electric circuit similar to Earth’s, and the likelihood of meeting these conditions in other planetary atmospheres, are briefly discussed. Atmospheric electrification could be important throughout the solar system, particularly at the outer planets which receive little solar radiation, increasing the relative significance of electrical forces. Nucleation onto atmospheric ions has been predicted to affect the evolution and lifetime of haze layers on Titan, Neptune and Triton. Atmospheric electrical processes on Titan, before the arrival of the Huygens probe, are summarised. For planets closer to Earth, heating from solar radiation dominates atmospheric circulations. However, Mars may have a global circuit analogous to the terrestrial model, but based on electrical discharges from dust storms. There is an increasing need for direct measurements of planetary atmospheric electrification, in particular on Mars, to assess the risk for future unmanned and manned missions. Theoretical understanding could be increased by cross-disciplinary work to modify and update models and parameterisations initially developed for a specific atmosphere, to make them more broadly applicable to other planetary atmospheres.     

Errors due to the anisotropic-common-ray approximation of the coupling ray theory

The common-ray approximation eliminates problems with ray tracing through S-wave singularities and also considerably simplifies the numerical algorithm of the coupling ray theory for S waves, but may introduce errors in travel times due to the perturbation from the common reference ray. These travel-time errors can deteriorate the coupling-ray-theory solution at high frequencies. It is thus of principal importance for numerical applications to estimate the errors due to the common-ray approximation applied. The anisotropic-common-ray approximation of the coupling ray theory is more accurate than the isotropic-common-ray approximation. We derive the equations for estimating the travel-time errors due to the anisotropic-common-ray (and also isotropic-common-ray) approximation of the coupling ray theory. The errors of the common-ray approximations are calculated along the anisotropic common rays in smooth velocity models without interfaces. The derivation is based on the general equations for the second-order perturbations of travel time.     

PS转换波界面二次源法射线追踪

界面二次源法是最近提出的一种最小走时射线追踪方法，尤其适合层状介质中走时和射线路径的计算.该方法相对于传统的最小走时树方法（如Moser法），仅在物性界面上设置二次源，射线路径的方向只在层界面处发生改变，该方法最大程度地消除了射线路径的锯齿状现象，同时也避免了低变速区的射线路径多值现象，因此，它具有更高的追踪精度和效率.本文采用界面二次源法在各向同性介质中实现了PS转换波射线追踪，理论模型的计算证实了界面二次源法追踪PS转换波的准确性和高效性，同时该方法在各向异性介质中也很好地追踪出分离的PSV波和PSH波，因此该方法有利于横波分裂在地震勘探中的研究和应用     

我国宇宙线空间物理学的进展

本文介绍了宇宙线空间物理学在我国的形成和主要研究内容,包括:(1)空间探测,有火箭探测、卫星探测;地面宇宙线台站观测;宇宙线的水下测量;(2)宇宙线空间物理学研究,有宇宙线的日地传输;宇宙线强度变化与CME事件;宇宙线的源物质与加速过程;宇宙线的地球物理效应.最后提到宇宙线与人体健康,特别是流行性感冒、大的太阳质子事件与地震现象、太阳宇宙线事件与天气和气候等的统计研究.     

新疆伽师强震群区基底界面结构特征

用射线分布分析法对伽师强震群区的高分辨折射地震剖面资料进行了更进一步的分析处理， 得到了伽师强震群区更完整的基底界面结构特征. 结果表明，在伽师强震群区地壳上部存在两个明显的结构界面:第一个界面的结构连续、完整，其埋深变化不大， 在2.6～3.3 km之间，为一向天山方向逐渐抬升、 近平直的倾斜界面；第二个界面的埋深变化较大， 在8.5～11.8 km之间，为古老的塔里木盆地结晶基底. 在约37 km桩号附近结晶基底有近2.5 km的深度突变， 推断可能是伽师强震群区超基底断裂所致. 以该断裂为界，结晶基底分为西南、东北两段. 每段内界面的埋深变化不大， 西南段的埋深约11.5 km， 东北段的埋深约为8.5～9.0 km，该段在从西南向东北整体抬升的背景上略有上隆，反映出在塔里木地块西北缘特殊的构造环境下上部地壳的变形特征.      

InSAR高程模型及其精度分析

提出了一种改进的InSAR高程模型，建立了高程和干涉相位的直接关系，并对公式推导中一般采用的平行射线近似处理方法所引入的高程误差进行了量化分析。结果表明，对于星载雷达而言，平行射线近似误差不能忽略。给出了近似误差与基线参数的确定性关系及相应的误差传播曲线，有助于误差纠正和重建高精度DEM。另外，基于改进的高程模型，推导出了高程测量误差传播公式，明确了基线长度和方向对测高精度的影响，对合理选择干涉像对具有指导意义。