Lithospheric magnetic anomalies in the territory of Siberia (from measurements by the CHAMP satellite)

The position of lithospheric magnetic anomalies, detected in total magnetic intensity and the vertical component of the magnetic field, has been determined for Siberia using data from the CHAMP satellite. The paper describes the technique for the satellite data processing and the ways of recognition of regional lithospheric magnetic anomalies from satellite-measured values of the total geomagnetic field, which are obtained from several sources (external and internal with respect to the Earth’s surface). Maps of magnetic-field anomalies of different scales have been constructed for several regions of Siberia depending on the method of areal averaging. The possible geologic and physical nature of the magnetic anomalies and their relationship with deep-seated crustal structures are considered. Preliminary interpretation of the magnetic-field maps shows that the anomalies are connected with the present-day large geologic and geophysical elements of the basement. The features of the lithospheric magnetic field, as a parameter reflecting the present position of tectonic structures and their physical properties, can be used for their contouring in combination with other geological and geophysical methods.     

Delineation of long-wavelength magnetic anomalies over central India by rectangular harmonic analysis

The method of rectangular harmonic analysis is applied to the geomagnetic field data from central India to isolate long wavelength magnetic anomalies associated with largescale crustal structures. The long-wavelength anomalies have accounted for approximately 20 % of the spatial variability of the residual magnetic field over the International Geomagnetic Reference Field. On the magnetic anomaly map, reflecting the surface expression of longwavelength anomalies, the Tapi-Narmada-Son zone is characterized by a feeble positive anomaly bounded by a strong negative anomaly. The anomaly pattern is believed to be caused by the large-scale undulation in Moho and related variations in the thickness of the lower (basaltic) crust. The other two prominent anomalies, the magnetic low striking northwest and the magnetic high trending east-northeast, appear to be related to the deep structural feature of the Godavari graben and the eastern Rajasthan lineament respectively.     

SMART-1 after lunar capture: First results and perspectives

SMART-1 is a technology demonstration mission for deep space solar electrical propulsion and technologies for the future. SMART-1 is Europe’s first lunar mission and will contribute to developing an international program of lunar exploration. The spacecraft was launched on 27th September 2003, as an auxiliary passenger to GTO on Ariane 5, to reach the Moon after a 15-month cruise, with lunar capture on 15th November 2004, just a week before the International Lunar Conference in Udaipur. SMART-1 carries seven experiments, including three remote sensing instruments used during the mission’s nominal six months and one year extension in lunar science orbit. These instruments will contribute to key planetary scientific questions, related to theories of lunar origin and evolution, the global and local crustal composition, the search for cold traps at the lunar poles and the mapping of potential lunar resources     

月球引力场和磁场探测新进展

简要地回顾了前苏联、美国探测月球引力场和磁场的历史,介绍了各国的探月计划;较详细地介绍和分析了美国克莱门汀(Clementine,Cl）和月球探测者(Lunar Prospector,LP)两艘飞船探测月球引力场和磁场的最新成果：Konopliv A S等根据月球探测者数据绘制的最新月球重力图(LP100j,月球正面n=90,背面n=60),Halekas J S等根据月球探测者电子反射测量数据绘制的第一张全月球磁场图,Zuber M T等根据克莱门汀数据制作的月球(自由空间和布格)重力异常图和月壳厚度图;提出了开展有关研究工作的几点建议。     

North-south asymmetry in response of geomagnetic activity to different solar events

Study of the response of geomagnetic activity to five different kinds of solar events reveals that an average north-south asymmetry of about 15% exists which diminishes with enhanced geomagnetic activity. The response of the geomagnetic field is quite significant only when high speed solar wind stream in association with sector boundary of interplanetary magnetic field (IMF) or solar proton streams near sector boundary sweeps past the earth. When the frequency of occurrence of indices of geomagnetic activity is considered, the index zero shows a marked difference in its response characteristics for the southern hemisphere. This appears to be a real feature and not attributable to any artefact of the index or its derivation.     

高空正常地磁场在航磁编图中的应用

在研究磁异常时,习惯将正常地磁场从测得的地磁场值中消除,以便突出上地幔和地壳内的各种磁异常。正常地磁场的选择正确与否,直接影响到人们对磁异常的认识及地质现象的研究。对于大面积的航空磁测编图,正常地磁场的选择尤为重要。     

Failed Eruptions of Solar Filaments

Solar filaments (prominences), which suddenly and swiftly ascend, i.e., become eruptive, sometimes decelerate and stop at comparatively low altitudes. Causes of failed eruptions generally remain uncertain. The present study analyzes two eruptive phenomena with very similar initial geometries and configurations of external magnetic fields; one of these eruptions evolves in a coronal mass ejection, but the other breaks off shortly after its start. The tension of curved magnetic field lines is the most probable force causing eruptions to stop. Significant external magnetic fields parallel to rope axes located in failed eruption regions can be a decisive factor. Such an effect has been revealed during laboratory experiments on plasma rope dynamics, which likely plays an important role in solar eruptive phenomena.     

The Nature of Variations in Anomalies of the Chemical Composition of the Solar Corona with the 11-Year Cycle

Evidence that the distribution of the abundances of admixtures with low first-ionization potentials (FIP < 10 eV) in the lower solar corona could be associated with the typology of the largescale magnetic field is presented. Solar observations show an enhancement in the abundances of elements with low FIPs compared to elements with high FIPs (>10 eV) in active regions and closed magnetic configurations in the lower corona. Observations with the ULYSSES spacecraft and at the Stanford Solar Observatory have revealed strong correlations between the manifestation of the FIP effect in the solar wind, the strength of the open magnetic flux (without regard to sign), and the ratio of the large-scale toroidal and poloidal magnetic fields at the solar surface. Analyses of observations of the Sun as a star show that the enhancement of the abundances of admixtures with low FIPs in the corona compared to their abundances in the photosphere (the FIP effect) is closely related to the solar-activity cycle and also with variations in the topology of the large-scale magnetic field. A possible mechanism for the relationship between the FIP effect and the spectral type of a star is discussed in the framework of solar–stellar analogies.     

Low energy neutral atom imaging on the Moon with the SARA instrument aboard Chandrayaan-1 mission

This paper reports on the Sub-keV Atom Reflecting Analyzer (SARA) experiment that will be flown on the first Indian lunar mission Chandrayaan-1. The SARA is a low energy neutral atom (LENA) imaging mass spectrometer, which will perform remote sensing of the lunar surface via detection of neutral atoms in the energy range from 10 eV to 3 keV from a 100km polar orbit. In this report we present the basic design of the SARA experiment and discuss various scientific issues that will be addressed. The SARA instrument consists of three major subsystems: a LENA sensor (CENA), a solar wind monitor (SWIM), and a digital processing unit (DPU). SARA will be used to image the solar wind-surface interaction to study primarily the surface composition and surface magnetic anomalies and associated mini-magnetospheres. Studies of lunar exosphere sources and space weathering on the Moon will also be attempted. SARA is the first LENA imaging mass spectrometer of its kind to be flown on a space mission. A replica of SARA is planned to fly to Mercury onboard the BepiColombo mission.     

External field characterization using CHAMP satellite data for induction studies

Knowledge of external inducing source field morphology is essential for precise estimation of electromagnetic (EM) induction response. A better characterization of the external source field of magnetospheric origin can be achieved by decomposing it into outer and inner magnetospheric contributions, which are best represented in Geocentric Solar Magnetospheric (GSM) and Solar Magnetic (SM) reference frames, respectively. Thus we propose a spherical harmonic (SH) model to estimate the outer magnetospheric contribution, following the iterative reweighted least squares approach, using the vector magnetic data of the CHAMP satellite. The data covers almost a complete solar cycle from July 2001 to September 2010, spanning 54,474 orbits. The SH model, developed using orbit-averaged vector magnetic data, reveals the existence of a stable outer magnetospheric contribution of about 7.39 nT. This stable field was removed from the CHAMP data after transforming to SM frame. The residual field in the SM frame acts as a primary source for induction in the Earth. The analysis of this time-series using wavelet transformation showed a dominant 27-day periodicity of the geomagnetic field. Therefore, we calculated the inductive EM C-response function in a least squares sense considering the 27-day period variation as the inducing signal. From the estimated C-response, we have determined that the global depth to the perfect substitute conductor is about 1132 km and its conductivity is around 1.05 S/m.     

Solar Wind Magnetic Field Turbulence over the Solar Activity Cycle Inferred from Coronal Sounding Experiments with Helios Linear-Polarized Signals

Results of experiments on polarized radio sounding of the outer solar corona using the Helios spacecraft from 1975 to 1984 are presented. The characteristic parameters of the temporal spectra of fluctuations in the Faraday rotation of the plane of polarization for heliocentric distances from 3.5 to 5.5 solar radii are obtained. The absolute level of these fluctuations and, consequently, the level of fluctuations of the magnetic field, is almost independent of the solar activity. It is well known that the global structure of the solar wind varies with the solar cycle such that there is slow solar wind at low latitudes and fast solar wind at high latitudes during solar minima. In contrast, a slow solar wind dominates at all latitudes during solar maxima. One explanation for the invariance of the fluctuations observed by sounding the circumsolar plasma is that the mean magnetohydrodynamic turbulence of the low-latitude, slow solar wind depends weakly on the phase of the solar cycle.

     

月球表面的环境特征

本文通过对月球探测资料和研究结果的系统分析,认为月球体积小、质量轻、离太阳较近(温度高)等因素是月球只有极为稀薄大气层的原因;论证了月球极地阴影区存在水冰的证据,并计算出水资源量约为66亿吨。研究了月壤中氦-3的含量与月壤颗粒大小、矿物组成、元素成分和结构特征的关系,并估算了氦-3的资源量;探讨了月球表面的反射率;综合分析了月球区域性磁场的形成机制。     

月球磁学观测与研究进展

月球磁场观测一直是月球研究的重要内容。20世纪六七十年代,通过绕月小卫星、Apollo登月及返回样品等观测实验,月球磁学研究已取得一系列重要进展,九十年代末期Lunar Prospector（LP）获得了月球的全球磁异常分布图。本文主要评述前人已取得的重要进展,重点讨论月球样品的剩磁来源、月球磁场古强度和发电机争论及其月球演化意义。     

Long and short term relationships between solar wind velocity and geomagnetic field at low latitudes

Solar wind velocity control of low latitude geomagnetic field both on long and short term basis is studied. It is shown that semiannual averages of the low latitude field is inversely related to solar wind velocity and that there is a dominant local time dependence of the relationship. Strongest correlation are confined to the local afternoon hours. It is also shown that for a duration when the solar wind velocity exhibits significant recurrent pattern the low latitude geomagnetic field also depicts strong solar synodic rotation periodicity of 27 days with significant coherence with velocity. The low latitude field on a short term basis is influenced by variable solar wind velocity with a delay of about 1–2 days. During the period of systematic recurrent pattern in solar wind velocity even the quiet-time night field at equatorial and low latitudes show a strong dependence on velocity indicative of the solar wind control of the quiet-time proton belt encompassing the earth.     

APPLICATION OF MAGNETOMETRIC DATA IN THE STUDY OF DEEP CRUSTAL STRUCTURE IN PLATFORM PROVINCES

Results of regional geophysical work in the U.S.S.R. allow a measure of correlation between the known structural features of the crust and those of the geomagnetic field. The “normal” magnetic field used for identifying magnetic anomalies is obtained by graphic smoothing of isolines of total intensity T. Detailed analysis of data obtained in aeromagnetic and gravity surveys throughout the U. S. S. R. leads to the conclusion that the cause of the observed regional magnetic and gravity anomalies lies in the same associated geologic objects located at the same level - that of a magnetoactive interval of the crystalline envelope of the earth. The conclusions that can be drawn from existing data are: 1) the existence of “continental” anomalies of the geomagnetic field cannot be explained as an effect of the crust; 2) the basaltic layer does not affect the distribution of the geomagnetic field; 3) the anomalies in the basic (normal) geomagnetic field are caused by the presence of thermomagnetic geologic bodies in the granitic layer; accordingly, it is theoretically possible to determine the thickness of the continental layer from magnetometric data. A table showing correlative depths of the basaltic layer, its thickness, and anomalous magnetic field, as well as magnetic profiles is included.--C. E. Sears.     

A Green’s function method for calculating the potential magnetic field in solar active regions in a spherical geometry

A Green’s function solution of Laplace’s equation for the potential magnetic field in an external spherical region is found using the derivative of the potential along a selected direction as a boundary condition. A set of programs applying this solution to construct the potential magnetic-field lines in solar active regions based on the photospheric line-of-sight field component has been developed. The method is tested using some model fields, and the optimal step size is found for realistic conditions. The developed software is applied to four real solar active regions, adopting HMI/SDO magnetograms as the boundary conditions. The potential magnetic field in the chromosphere and corona have been reconstructed for the selected regions. The calculated field lines are compared with flux tubes observed by AIA/SDO in the EUV. This comparison is used as a basis to discuss the applicability of a potential field approximation to the magnetic fields in solar active regions.     

Moons' magnetism: from Io's and Ganymede's present magnetic signatures to the ancient lunar dynamo

Intrinsic magnetic fields, corresponding to virtual axial dipole moments of the order of 10²⁰ Am², have recently been evidenced for the Jovian satellites Io and Ganymede. By reviewing the rock magnetic and palaeomagnetic properties together with the history of Io, the hypothesis of a moment due to induced or remanent magnetization of crustal rocks acquired within the ambient Jovian field is clearly eliminated. This demonstration is all the more valid for Ganymede, which experiences a much lower Jovian field. The demonstration of a present dynamo action for these Jovian moons, possibly sustained by Jupiter through tidal heating and background magnetic field, may be an actualistic model for the early lunar history. The hypothesis of a lunar dynamo, active at 3–4 Ga, seems to be strongly supported by this analogy.     

Tectonomagnetic study in the seismoactive area of Narmada-Son lineament,central India: Preliminary results on repeat field observations

Repeated measurements of the total geomagnetic field on the five profiles have revealed a picture of stress-induced tectonomagnetic effect in the form of secular variation of the total geomagnetic field in the tectonically and seismically active area of Jabalpur and adjoining areas of the Narmada-Son lineament (NSL), central India. For this experiment, a reference base station was established within the study area at Jabalpur. Using proton precession magnetometers with a sensitivity of 0.1 nT, simultaneous measurements of total geomagnetic field were made annually at the base and all field stations. Five cycles of repeated observations have been performed between 2003 and 2007. For data analysis, a difference method has been applied and the residuals have been calculated as secular variations of the total geomagnetic field with values ranging from ±0.1nT to about ±14.6nT/yr over the different stations. The anomalies in secular variation of the total geomagnetic field may be related to anomalous accumulation of tectonic stresses and tensions on the deep fault zones and crustal blocks due to recent geodynamic processes and active geological inhomogeneities in the NSL.