根据三斜距确定点的三维坐标及精度

本文绘出一种根据三斜距解算点的三维坐标的直接方法,无需初值、迭代及多值判断,非常适合计算机编程;给出的实用精度估算式能方便地实现根据三斜里估算待定点三维点位精度之目的;对其应用条件的讨论,提出了应用中的具体倾角限值,对指导实际工作具有重要意义。     

POLAR spacecraft observations of helium ion angular anisotropy in the Earth’s radiation belts

New observations of energetic helium ion fluxes in the Earth’s radiation belts have been obtained with the CAMMICE/HIT instrument on the ISTP/GGS POLAR spacecraft during the extended geomagnetically low activity period April through October 1996. POLAR executes a high inclination trajectory that crosses over both polar cap regions and passes over the geomagnetic equator in the heart of the radiation belts. The latter attribute makes possible direct observations of nearly the full equatorial helium ion pitch angle distributions in the heart of the Earth’s radiation belt region. Additionally, the spacecraft often re-encounters the same geomagnetic flux tube at a substantially off-equatorial location within a few tens of minutes prior to or after the equatorial crossing. This makes both the equatorial pitch angle distribution and an expanded view of the local off-equatorial pitch angle distribution observable. The orbit of POLAR also permitted observations to be made in conjugate magnetic local time sectors over the course of the same day, and this afforded direct comparison of observations on diametrically opposite locations in the Earth’s radiation belt region at closely spaced times. Results from four helium ion data channels covering ion kinetic energies from 520 to 8200 KeV show that the distributions display trapped particle characteristics with angular flux peaks for equatorially mirroring particles as one might reasonably expect. However, the helium ion pitch angle distributions generally flattened out for equatorial pitch angles below about 45°. Significant and systematic helium ion anisotropy difference at conjugate magnetic local time were also observed, and we report quiet time azimuthal variations of the anisotropy index.     

Possible configurations of the magnetic field in the outer magnetosphere during geomagnetic polarity reversals

Possible configurations of the magnetic field in the outer magnetosphere during geomagnetic polarity reversals are investigated by considering the idealized problem of a magnetic multipole of order m and degree n located at the centre of a spherical cavity surrounded by a boundless perfect diamagnetic medium. In this illustrative idealization, the fixed spherical (magnetopause) boundary layer behaves as a perfectly conducting surface that shields the external diamagnetic medium from the compressed multipole magnetic field, which is therefore confined within the spherical cavity. For a general magnetic multipole of degree n, the non-radial components of magnetic induction just inside the magnetopause are increased by the factor 1 + [(n + 1)/n] relative to their corresponding values in the absence of the perfectly conducting spherical magnetopause. An exact equation is derived for the magnetic field lines of an individual zonal (m = 0), or axisymmetric, magnetic multipole of arbitrary degree n located at the centre of the magnetospheric cavity. For such a zonal magnetic multipole, there are always two neutral points and n – 1 neutral rings on the spherical magnetopause surface. The two neutral points are located at the poles of the spherical magnetopause. If n is even, one of the neutral rings is coincident with the equator; otherwise, the neutral rings are located symmetrically with respect to the equator. The actual existence of idealized higher-degree (n > 1) axisymmetric magnetospheres would necessarily imply multiple (n + 1) magnetospheric cusps and multiple (n) ring currents. Exact equations are also derived for the magnetic field lines of an individual non-axisymmetric magnetic multipole, confined by a perfectly conducting spherical magnetopause, in two special cases; namely, a symmetric sectorial multipole (m = n) and an antisymmetric sectorial multipole (m = n – 1). For both these non-axisymmetric magnetic multipoles, there exists on the spherical magnetopause surface a set of neutral points linked by a network of magnetic field lines. Novel magnetospheric processes are likely to arise from the existence of magnetic neutral lines that extend from the magnetopause to the surface of the Earth. Finally, magnetic field lines that are confined to, or perpendicular to, either special meridional planes or the equatorial plane, when the multipole is in free space, continue to be confined to, or perpendicular to, these same planes when the perfectly conducting magnetopause is present.Also Honorary Research Associate, Rutherford Appleton Laboratory, Chilton, Didcot, Oxon OX11 0QX, UK and Visiting Reader in Physics. University of Sussex, Falmer, Brighton BN1 9QH, UK     

Stationary magnetospheric convection on November 24, 1981. 1. A case study of “pressure gradient/minimum-B” auroral arc generation

We present two case studies in the night and evening sides of the auroral oval, based on plasma and field measurements made at low altitudes by the AUREOL-3 satellite, during a long period of stationary magnetospheric convection (SMC) on November 24, 1981. The basic feature of both oval crossings was an evident double oval pattern, including (1) a weak arc-type structure at the equatorial edge of the oval/polar edge of the diffuse auroral band, collocated with an upward field-aligned current (FAC) sheet of ≈1.0 μA m⁻², (2) an intermediate region of weaker precipitation within the oval, (3) a more intense auroral band at the polar oval boundary, and (4) polar diffuse auroral zone near the polar cap boundary. These measurements are compared with the published magnetospheric data during this SMC period, accumulated by Yahnin et al. and Sergeev et al., including a semi-empirical radial magnetic field profile B_Z in the near-Earth neutral sheet, with a minimum at about 10–14 R_E. Such a radial B_Z profile appears to be very similar to that assumed in the “minimum B/cross-tail line current” model by Galperin et al. (GVZ92) as the “root of the arc”, or the arc generic region. This model considers a FAC generator mechanism by Grad-Vasyliunas-Boström-Tverskoy operating in the region of a narrow magnetic field minimum in the near-Earth neutral sheet, together with the concept of ion non-adiabatic scattering in the “wall region”. The generated upward FAC branch of the double sheet current structure feeds the steady auroral arc/inverted-V at the equatorial border of the oval. When the semi-empirical B_Z profile is introduced in the GVZ92 model, a good agreement is found between the modelled current and the measured characteristics of the FACs associated with the equatorial arc. Thus the main predictions of the GVZ92 model concerning the “minimum-B” region are consistent with these data, while some small-scale features are not reproduced. Implications of the GVZ92 model are discussed, particularly concerning the necessary conditions for a substorm onset that were not fulfilled during the SMC period.     

Substorm observations in the early morning sector with Equator-S and Geotail

Data from Equator-S and Geotail are used to study the dynamics of the plasma sheet observed during a substorm with multiple intensifications on 25 April 1998, when both spacecraft were located in the early morning sector (03–04 MLT) at a radial distance of 10–11 R_E. In association with the onset of a poleward expansion of the aurora and the westward electrojet in the premidnight and midnight sector, both satellites in the morning sector observed plasma sheet thinning and changes toward a more tail-like field configuration. During the subsequent poleward expansion in a wider local time sector (20−04 MLT), on the other hand, the magnetic field configuration at both satellites changed into a more dipolar configuration and both satellites encountered again the hot plasma sheet. High-speed plasma flows with velocities of up to 600 km/s and lasting 2–5 min were observed in the plasma sheet and near its boundary during this plasma sheet expansion. These high-speed flows included significant dawn-dusk flows and had a shear structure. They may have been produced by an induced electric field at the local dipolarization region and/or by an enhanced pressure gradient associated with the injection in the midnight plasma sheet.     

古冲沟冲积扇体地震反射资料研究

利用地震资料研究古冲沟冲积扇体的反射特征、内部结构、剖面特征和分布特征等问题,研究结果为识别和确认古冲沟冲积扇体油气藏提供依据     

地理信息系统（GIS）科学体验区建设

针对国内缺少面向非专业人群的GIS科普内容的状况,研究在建构主义体验学习与情境学习理论的指导下,提出了＂以兴趣引导体验促科学知识发现＂的GIS体验区建设理念,形成了＂掌握空间分析方法、提高动手实践能力、转变思维方式和观念＂的体验目标和＂用半开放体验线路串联系列小案例反映GIS方法与应用＂的设计思路,进而以＂GIS知识学习——GIS初步应用——GIS项目选址＂为体验主线,进行了GIS体验区的框架设计和分场景设计,并综合运用RIA技术和开源WebGIS技术,构建了GIS科学体验的数字互动平台。GIS体验区网站运行一年以来,访问量超过17万人次,结果表明,GIS体验区能够有效把握体验者的兴趣,有利于推动GIS的大众化发展。     

中国地质学会第一届科普奖揭晓

正为了进一步加强地质学科学普及,鼓励会员参与地质科普,中国地质学会设立了科普奖。中国地质学会第一届科普奖近日揭晓,5位科学家获人物奖,5组作品获产品奖。该获奖名单是由各省级地质学会和中国地质学会各专业委员会推荐,经专家评选后确定,并于2020年4月21日～26日在中国地质学会网站公示。     

从传播学仪式观理论视角探讨防震减灾科普宣传的参与实践——以云南防震减灾科普民歌为例

受众参与是防震减灾科普宣传工作的重要基础。从传播学仪式观的理论视角,以云南防震减灾科普民歌为案例,提出在云南少数民族地区有效开展防震减灾科普宣传工作的对策建议:①细分受众,有针对性地开展防震减灾科普宣传;②强调受众参与,强化防震减灾科普宣传实效;③创新形式,依托少数民族地区喜闻乐见的文艺体现形式开展防震减灾科普宣传。     

南堡1号构造馆三段断盖配置油气渗漏部位及其控藏作用

为了研究南堡凹陷南堡1号馆三段火山岩盖层上下油气分布规律,在馆三段火山岩盖层及其内油气渗漏断裂发育及分布特征研究的基础上,通过对馆三段火山岩盖层断接厚度与其封油气所需最小断接厚度相对大小的比较和对油气渗漏断裂凸面脊的确定,预测了南堡1号构造馆三段断盖配置油气渗漏部位;并结合油气分布,对断盖配置油气渗漏部位对油气成藏与分布的控制作用进行了研究。结果表明,南堡1号构造馆三段断盖配置发育10处油气渗漏部位,其中：F₂及分支断裂油气渗漏部位最发育,有3处油气渗漏部位;其次是F₁、F₆断裂,有2处油气渗漏部位;F₃、F₄、F₅和F₇断裂仅各发育1处油气渗漏部位。这些油气渗漏部位及附近有利于下伏东一段油气在上覆馆三段之上聚集成藏,应是造成南堡1-1断鼻、南堡1-3断块和南堡1-5断鼻北部油区油气既可以分布在下伏东一段又可分布在馆三段之上,而南堡1-5断鼻南部油气仅分布在下伏东一段的根本原因。