带电月尘活动对月球磁场的影响

本文介绍了基于月尘扬起机制的"动态喷泉模型",分析了月尘扬起的过程;最后提出了"带电月尘活动电磁感应模型",计算得到月面明暗交界处带电月尘活动产生的感应磁场强度小于0.0064nT.本文证明带电月尘的活动对月球磁场的影响微小,可以忽略.     

月球磁场研究新进展

月球磁场是探索月球起源的重要渠道,也是研究地月体系及太阳系运转模式的一个重要方面.本文介绍了第40届国际月球与行星科学大会盛况,根据会议信息,阐述了月球磁场研究的现状、取得的新进展和有待于突破的重要问题;同时分析了月球磁场研究的重要性,并展望了未来月球磁场研究的方向.     

月球重力场对月球内部结构研究的作用

月球是人类深空探测的首要目标,而月球的内部结构则是我们了解月球与地月系形成与演化的重要窗口.相比于其他物理场,月球重力场模型具有全球均匀覆盖、精度和分辨率持续提高的特点,在月球内部结构研究中扮演着重要作用.本文对月球重力场在月球内部结构研究中发挥的作用进行了论述,包括月壳、月幔以及月核,其中重点介绍了高阶次重力场模型对...     

对月球重力场特征的理解

依据克莱门汀号和月球勘探者号月球探测器所获得的数据所建立最新的地球重力模型和地形模型，为人类深入了解月球内部性质及其演化特征，提供新的平台.M.T. Zuber (1994) 和 M. A. Wieczorek (1998) 所建立的月壳全球模型，为利用最新月球着力资料研究月球内部构造和演化，揭示月球上独特的“物质瘤”之成因等科学问题，开凿了先河.本文通过对现有的月球重力和地形数进行分析和计算，提出作者对月球内部物质分布特征的理解和一些认识.从宏观角度看，月球布格重力异常与月球地形起伏是相关的，统计结果表明它们呈弱负相关，从均衡角度来说，在月球停止大规模内部物质运动之前，月球壳幔可能已基本达到均衡；从Mascon深度估算结果来看，一些大型的Mascon基本属于玄武岩浆“充填”型的，少数Mascon可能与月幔柱有关，如东方海Mascon.     

月球表层及月壳物质密度分布特征

月球表层与月壳岩石密度的横向与径向的变化,反映了月表及内部成分以及月球演化等特征.本文利用月球勘探者号伽马射线谱仪探测的月表Fe, Th与Mg元素分布数据,依据前人给出的元素含量与岩石类型的关系,对月球表层进行了岩性填图,并结合岩石样品与陨石的密度测试数据建立初始密度模型,采用铁元素与岩石密度的关系对其进行修正,从而建立了月表物质密度分布模型.基于嫦娥一号激光测高数据和日本SELENE计划发布的月球重力模型,计算出月球布格重力异常,进而反演得到月壳0~40 km深度范围内岩石平均密度分布模型.分析表明,大部分区域上,月壳至少月壳上部岩石成分主要以轻质的富含铝、钙、镁质的硅酸盐类岩石为主.由此推测,原始月壳极有可能是由轻质的、富含钙、镁质硅酸盐类岩石构成的全球性月壳.现今的玄武岩与克里普岩只是覆盖于原始的月壳之上的岩层,且厚度不大.     

干旱、地震与月球赤纬角变化

计算了月球赤纬角最大和最小时地球的潮汐形变值．结果表明,当赤纬角最大时月球引潮力所引起的地球表面积和地壳容积变化量是赤纬角最小时所引起的相应变化量的２．３倍．因此,当月球赤纬角最大时地球大量放气,而月球赤纬角最小时气候干旱,中国大陆出现旱灾．用地球自转速度变化周期和地震周期对上述结论进行了论证．     

月球探测及月球重力场的确定

针对近年月球探测渐成热点和我国即将发射“嫦娥卫星”的状况，本文首先归纳了月球各项几何与物理特性以及月球探测的经济、科学和战略意义.然后，讨论了月球重力场在探月中的作用，并对国外月球重力场研究的发展历程、主要方法及面临的困难进行了综述.最后，结合我国“嫦娥工程”，对我国月球重力场探测的可行性，从航天运载能力、轨道跟踪手段、重力场恢复技术以及方法创新等方面进行了分析，以期为我国自主确定月球重力场模型提供参考依据.     

月球富钛玄武岩喷发对月球生热元素丰度的约束

近几十年来,对月球的遥感观测以及对月岩样品的分析揭示了月海玄武岩、镁铁质月球玻璃等的时间和空间分布特征,其被认为与月幔的热化学演化密切相关,并且引出了许多解释模型.本文考虑月球结晶末期在上部形成的致密的钛铁矿层和下部的月幔,由于密度原因钛铁矿层发生倒转,之后受热上涌产生玄武质岩浆等的演化过程,从热化学演化的角度为月海玄...     

月球南北两极研究进展与发展趋势

本文着重对上世纪90年代开始的对月探测中关于月球南北两极的一些研究结果进行了综述，包括地质地貌，水冰及其光照条件等问题.笔者认为，在未来的对月球两极的探测活动中，获取月球两极更高空间分辨率的地形和地质等数据是非常重要的，而与此相关的光照，温度及同月球基地建设相关问题等研究将是主要的研究方向，且必将随着各国探测进程的发展取得更多和更深刻的认识.     

琼中地磁台磁场变化特征及其与区域磁场的关系

对琼中地磁台台址及邻域10年来磁场监测资料进行分析,查明:a、台址位于海南岛区域磁场背景值变化转折处附近的弱磁性异常区中;b、台址磁场均匀,台址周围5km范围内磁场各要素的差值ΔF<80~(nT)、ΔH<70~(nT)、ΔZ<-200~(nT);c、全岛21个测点的实测平均值减去本台观测值得ΔD=0′.0、ΔF=-120~(nT)、ΔH=-42~(nT)、Δ=-144~(nT);d、距台站100m以外的其他人为铁磁性干扰源对本台的观测值不明显。由此说明本台的地磁观测资料能真实反映当地磁场特征及其变化。本台可作观测海南岛区域磁场变化的窗口。     

Constraints on the origins of lunar magnetism from electron reflection measurements of surface magnetic fields

Apollo 15 and 16 subsatellite measurements of lunar surface magnetic fields by the electron reflection method are summarized. Patches of strong surface fields ranging from less than $\text{1}\text{4}$° to tens of degrees in size are found distributed over the lunar surface, but in general no obvious correlation is observed between field anomalies and surface geology. In lunar mare regions a positive statistical correlation is found between the surface field strength and the geologic age of the surface as determined from crater erosion studies. However, there is a lack of correlation of surface field with impact craters in the mare, implying that mare do not have a strong large-scale uniform magnetization as might be expected from an ancient lunar dynamo. This lack of correlation also indicates that mare impact processes do not generate strong magnetization coherent over ～ 10 km scale size. In the lunar highlands fields of >100 nT are found in a region of order 10 km wide and >300 km long centered on and paralleling the long linear rille, Rima Sirsalis. These fields imply that the rille has a strong magnetization (>5 × 10^?6 gauss cm³ gm^?1 associated with it, either in the form of intrusive, magnetized rock or as a gap in a uniformly magnetic layer of rock. However, a survey of seven lunar farside magnetic anomalies observed by the Apollo 16 subsatellite suggests a correlation with inner ejecta material from large impact basins. The implications of these results for the origin of lunar magnetism are discussed.     

福州盆地全新世沉积物的磁学性质及其对环境变化的响应

福州盆地位于海陆过渡地带,在海陆变迁过程中,沉积物记录了高分辨率的环境信息,是揭示沉积特征对环境变化响应过程及模式的理想区域.本文选择位于福州盆地的FZ5钻孔进行岩石磁学、环境磁学和古地磁学方面的研究,以期阐明该区域沉积物磁学性质对陆源碎屑输入、海平面变化和成岩作用的响应.岩石磁学结果表明钻孔沉积物以低矫顽力的亚铁磁性矿物为主体,但是在不同的环境变化阶段,磁性矿物的类型有较大变化.在9~3 cal. ka BP的海侵过程中,沉积物中以磁铁矿为主体,存在菱铁矿和铁硫化物等还原性矿物.硫化作用使细粒磁铁矿溶解形成胶黄铁矿和黄铁矿,其峰面随碎屑磁性矿物的浓度变化而迁移.但硫化作用没有完全消除磁铁矿携带的特征剩磁和陆源碎屑输入量以及海平面升降对该阶段沉积物磁性的控制.在~3 cal. ka BP以来随着海平面下降、沉积环境向陆相氧化环境转化,虽然早期还原作用仍然存在,但后期氧化作用使磁性矿物向高矫顽力的赤铁矿等矿物转变,氧化作用基本扰乱了磁铁矿携带的剩磁.沉积及其后期成岩作用过程中,发生在约~8.2、~7.7、~7.5、~2.7、~1.5、~0.5 cal. ka BP六次强烈的古氧化界面反映了福州盆地当时异常干旱或湿热的气候事件.     

Textural remanence: A new model of lunar rock magnetism

In reexamining the accumulated magnetic data on lunar rocks, several common patterns of magnetic behavior are recognized. Their joint occurrence strongly suggests a new model of lunar rock magnetism, which appeals only to partial preferred textural alignment of the spontaneous moments of magnetic grains, without requiring the existence of ancient lunar magnetic fields. This magnetic fabric, mimetic to locally oriented petrofabric, gives rise to an apparent “textural remanent magnetization” (TXRM). In order to account for the observed intensity of “stable remanence” in lunar rocks, only a minute fraction (10^?3 to 10^?5) of the single-domain iron grains present need be preferentially aligned. Several mechanisms operating on the lunar surface, including shock and diurnal thermal cycling, appear adequate for producing the required type and degree of magnetic alignment in all lunar rock classes. The model is supported by a wide variety of direct and indirect evidence and its predictions (e.g. regarding anisotropic susceptibility and remanence acquisition) can be experimentally tested.     

Past and present magnetism of the Moon

The characteristics of the remanent magnetism of lunar samples suggests that it was acquired in a magnetic field on the Moon. The most likely origin of the field is a dynamo process in a molten, electricallyconducting core, but generation of a transient magnetic field during large meteorite impacts cannot be entirely ruled out. The magnetizing process may be thermoremanence, acquired when the rocks cooled through, the Curie point of the constituent iron grains which carry the remanent magnetization, or it may involve shock at the time of a meteorite impact, with or without a partial thermoremanence arising from heating.Evidence from absolute and relative determinations of the ancient field strength from the sample magnetizations strongly favours a global lunar field. This is implied by a trend which shows the field rising to a maximum value of 100 T between about 3.9–3.7 by ago and then decaying to 5–10 T until3.1 by. Such a systematic variation of field with time is not expected to be derived from magnetizations acquired in transient, impact-generated fields varying randomly in intensity.Contributory evidence for a dynamo field is provided by measurements of present lunar surface fields, the present very small dipole moment of the Moon and accumulating evidence of variation of the axis of the lunar field with time. Although there is no direct evidence for the existence of a lunar core the relevant observations are consistent with the presence of a core of up to 400 km, in radius. There are some difficulties associated with the lunar dynamo mechanism and its energy source but the evidence for a lunar dynamo is accumulating, with important implications for the structure and thermal history of the Moon.     

环境磁学在城市环境污染监测中的应用和进展

环境磁学是一门介于地球科学、环境科学和磁学之间的边缘科学，已广泛应用于很多领域.本文在简述了环境磁学参数和不同环境中磁性矿物变迁和演化过程的基础上,介绍了环境磁学在城市环境污染的不同方面所取得的进展,探讨了环境磁学在土壤污染和大气等城市环境污染研究中的不足,提出了环境磁学在城市环境污染研究领域的发展趋势.     

Test of IGRF (1980) main field and secular variation in Europe

The IGRF-models for the main field and the secular variation (IGRF 1980 and IGRF-SV 1980–1985) have been compared with geomagnetic ground based data for epoch 1980.5 in the GDR, and also with the secular variation at 34 European observatories. The results for the main magnetic field were much better than for IGRF 1965. With a level-error of ～ 45 nT, the IGRF 1980 included ～ 75% of the magnetic crust field. The structure of the IGRF-field is similar to that of other regional reference fields.The IGRF-SV for 1965, 1975 and 1980–1985 have been compared with analytical SV-models, based on low-degree polynomial approximations. It is shown that the main features of SV in Europe are represented correctly. The mean differences between observatory data and IGRF-SV 1980–1985 are 1.5′/a for declination, and 7 nT/a for total intensity.     

1900-2000年非偶极子磁场的全球变化

根据第７代ＩＧＲＦ模型,计算并绘制了１９００-２０００年（时间间隔为５ａ）非偶极子磁场的全球分布,计算和分析了各个磁异常中心位置和强度的变化,东亚正磁异常、大洋洲负磁异常、南大西洋正磁异常、非洲负磁异常和北美洲正磁异常是分布范围广、异常强度大的５个磁异常。南大西洋正磁异常是强度最大的磁异常。在２０世纪９０年代以前,东亚正磁异常的强度位居第２位,９０年代以后,非洲负磁异常的强度（绝对值）超过东亚正磁异常,成为第２大磁异常。磁异常强度增长最快的是非洲负磁异常、南大西洋正磁异常和大洋洲负磁异常。南大西洋正磁异常和非洲负磁异常是磁异常中心位置变化最快的两个磁异常。     

月球射电探测仪天线特性分析

本文介绍月球射电探测仪的基本原理，通过讨论所使用的电偶极天线的特性，得到了月球地层上方不同频率及不同距地高度的天线方向图，为最终选择出最佳方案提供了参考.