南极冰雪及非南极地区尘粒的研究及其成因

南极冰、雪及冰川沉积物中，特别是在富集陨石的冰区内发现和收集了较大量的宇宙尘、微陨石及火山成因的尘粒带，在非南极地区的大气平流层和深海沉积物中也收集到了宇宙尘。按其宇宙尘分布特征划分为行星际宇宙尘和恒星际宇宙尘。按其成因将宇宙尘划分为彗星成因、小行星成因、陨石消融成因及恒星际成因或前太阳的尘粒或粒子，并提出了判别宇宙尘的综合标志，同时讨论了宇宙尘的成因     

极区上行离子对地磁活动和季节变化响应的统计分析

利用DMSP F13卫星离子漂移速度测量数据和Wind卫星行星际磁场测量数据,对极区顶部电离层离子整体上行进行研究,主要考察平静期和磁暴期离子上行强度,以及不同行星际磁场方向和季节对离子上行的影响。研究发现,无论是南半球还是北半球,磁暴期的上行发生率都超过平静期;无论磁暴期还是平静期,南半球在北向行星际磁场时上行发生率高于南向行星际磁场、北半球在南向行星际磁场时上行发生率高于北向行星际磁场,且该结论在磁暴期比平静期更为明显;南半球平静期在北向行星际磁场和南向行星际磁场时冬季的上行发生率都远高于夏季,超过2倍,北半球平静期在北向行星际磁场和南向行星际磁场时夏季的上行发生率高于冬季。     

A bimodal model of the solar wind speed

Until the ULYSSES spacecraft reached high latitude, the only means for measuring the solar wind velocity in the polar regions was from radio scattering observations (IPS), and these remain the only way to measure the velocity near the sun. However, IPS, like many remote sensing observations, is a line-of-sight integrated measurement. This integration is particularly troublesome when the line-of-sight passes through a fast stream but that stream does not occupy the entire scattering region. Observations from the HELIOS spacecraft have shown that the solar wind has a bimodal character which becomes more pronounced near the sun. Recent observations from ULYSSES have confirmed that this structure is clear at high latitudes even at relatively large solar distances. We have developed a method of separating the fast and slow contributions to an IPS observation which takes advantage of this bimodal structure. In this paper I will describe the technique and its application to IPS observations made using the receiving antennas of the EISCAT incoherent backscatter radar observatory in northern Scandinavia.     

Interactions of large meteoroids and small interplanetary bodies with the Earth's atmosphere: Theories and observational constraints

Problems of hypervelocity interaction of large bodies with the Earth's atmosphere has attracted more attention during last few years. Several new concepts of dynamical explosive fragmentation of strong interplanetary bodies at extremely low heights under dynamic pressures of hundreds of Mdyn/cm² were published. Comparison of these theoretical models with precise observations has not yet been done, because data on atmospheric penetration of large bodies are not available.Single body theory with sudden gross-fragmentation was successfully applied to photographic observations of fireballs. The largest bodies observed have sizes up to several meters. The highest dynamic pressure acting on these observed bodies reached slightly over 100 Mdyn/cm². All these photographed fireballs follow theoretical concepts of motion of either the single-body or the single-body with gross-fragmentation under dynamic pressures in the range from 1 to 12 Mdyn/cm². When this theory has been applied to photographic observations, typical standard deviation of the distance flown in the trajectory has been found in a range of 10 to 30 m for one observed distance corresponding also to the geometrical precision of the observations. This model can explain all good observations of atmospheric trajectories of meteoroids up to initial sizes of several meters with high precision. Also the three photographed and one videorecorded meteorite falls fit to this concept completely.The most important phenomenon of atmospheric motion of meteoroids up to several meters in size is the ablation with final stage of hot vapor from ablated material. Spectral records of meteoroids up to several meters in size, down to a height of 16 km and for various velocities show overwhelming radiation of rather low excited metalic atoms (several eV; temperatures 3000 to 5000 K) in the pass-band of visible light. Radiation from high excited atoms of either atmospheric or ablational origin forms only an insignificant part of visible radiation.Contrary to this regime, theories of very large bodies contain ablation mostly in the form of explosive fragmentation. Ablation at higher heights is negligible. This absence of classical ablation and fragmentation at low dynamic pressures for large bodies (contrary to observations of smaller bodies) brings the body to lower heights without too much change of size and makes thus the dynamic pressure much higher than in reality. In any case the change of body dynamics and radiation going from sizes of several meters (observed regime) to sizes of several tens of meters (hypothetical regime) may be crucial for our understanding of dynamics and radiation of large body penetration through the low atmosphere to the Earth's surface. Observations of atmospheric trajectory of these bodies with sufficiently high precision are extremely needed.     

Partial averaging near a resonance in planetary dynamics

An analytical treatment of the evolutionary dynamics of a three-body planetary system subject to dynamical friction with an interplanetary medium is presented. The analysis presented here is in connection with the results of numerical integrations of such systems recently published by Haghighipour. Using the method of partial averaging near a resonance, the dynamics of a restricted, circular, planar three-body system, with the inner body more massive, is studied and the time variation of quantities such as the orbital angular momentum and the eccentricity of the outer planet, which were previously obtained from numerical integrations, is analytically verified.     

Noble Gas Isotopic Compositions of Cobalt-rich Ferromanganese Crusts from the Western Pacific Ocean and Their Geological Implications

1 Introduction Submarine metallic mineral resources consist mainly of polymetallic nodules and cobalt-rich ferromanganese crusts. Despite being discovered much later than the former, the latter are becoming one of the most important submarine polymetallic ore resources, because they containmany valuable metallic elements such as Co, platinum group elements (PGE), rare earth elements (REE), Ni and Cu, besides high contents of Fe and Mn (He et al., 2001). The Co-rich crusts are widely distr…     

日侧弥散极光对太阳风动压增强的响应

太阳风动压的显著变化能导致沉降进入极区电离层的能量粒子通量以及磁层-电离层电流系发生扰动。磁层高能粒子沉降到极区上层大气并与中性气体碰撞所激发的弥散极光,能够对这种扰动做出相应的响应。基于斯瓦尔巴特（Svalbard）群岛新奥尔松（Ny-?lesund）地区北极黄河站优越的地理优势,我们利用安装在黄河站的极光全天空成像仪观测到了日侧弥散极光对太阳风动压增强的响应。通过2006年1月2日事件观测显示,随着太阳风动压的增强,日侧弥散极光在极光卵赤道向部分首先点亮并逐渐向高纬扩展,同时地磁环境也受到相应扰动影响。我们认为,随着太阳风动压的增强,日侧磁层顶受到压缩,磁层内波粒相互作用导致投掷角散射增强,使得沉降进入极光卵赤道侧电离层的高能粒子数密度增大,进而导致日侧弥散极光强度增强。     

不同行星际磁场条件下极向运动极光结构的多手段联合观测

本文利用北极黄河站三波段全天空成像仪（ASI）的高分辨率的地面极光观测数据,联合欧洲非相干散射雷达（EISCAT）Svalbard雷达（ESR）,超级双子极光雷达网（SuperDARN）雷达等观测,研究了发生在2003年12月22日0900-1010 UT时间段内极区电离层极光和等离子体的变化特征。研究发现在不同行星际磁场（IMF）条件下,黄河站极光ASI均观测到了一系列极向运动极光结构（PMAFs）,其特征为极光在赤道向一侧点亮后向高纬扩展。这些PMAFs都伴随有明显的粒子沉降特征,且在IMF北向时该粒子沉降能达到更低的电离层E层区域,而此时这些PMAFs相应位置的高纬电离层出现了一个典型反向对流涡,这是高纬（尾瓣）重联的典型特征之一。这些结果表明北向IMF条件下的这些PMAFs是由高纬重联所产生。在IMF南向时,黄河站观测到的PMAFs可跨越更广的地磁纬度,表明其演化时间亦较长,其相应区域的电离层特征也表明该PMAFs由日侧磁层顶低纬磁重联所产生。     

X-rays in the Solar System

Soft X-ray observations from comets are analysed on the assumption that the X-rays arise from electron captures by multiply charged ions of the solar wind in collisions with the neutral atoms and molecules of the cometary atmospheres. The collisions populate excited states of the ion formed in the transfer of charge which then decay in a cascade of radiative transitions in the soft X-ray and ultraviolet regions of the spectrum. A comparison of detailed models of the resulting spectra with observations of Comet McNaught-Hartley yield information on the solar wind ion composition. A similar process in which solar wind ions interact with neutral atoms in the heliosphere contributes to the diffuse soft X-ray background. This revised version was published online in July 2006 with corrections to the Cover Date.