中国地磁基本场模式建立方法探讨

利用７０年代的地磁资料，讨论了测点密度和测点坐标变换对建立中国地磁基本场模式的影响。结果表明，只选用分布较均匀的２００个左右的测点建立基本场模式是可行的；对测点的球面坐标进行Ｍｅｒｃａｔｏｒ投影变换是必要的，可以显著减小模式的场值分布在边界附近出现的畸变现象；３阶到５阶模式均主要反映正常的基本磁场分布，而５阶模式效果最好     

Sun,earth and sky

The Sun is enveloped by a hot, tenuous million-degree corona that expands to create a continuous solar wind that sweeps past all the planets and fills the heliosphere. The solar wind is modulated by strong gusts that are initiated by powerful explosions on the Sun, including solar flares and coronal mass ejections. This dynamic, invisible outer atmosphere of the Sun is currently under observation with the soft X-ray telescope aboard the Yohkoh spacecraft, whose results are presented. We also show observations from the Ulysses spacecraft that is now passing over the solar pole, sampling the solar wind in this region for the first time. Two other spacecraft, Voyager 1 and 2, have recently detected the outer edge of the invisible heliosphere, roughly halfway to the nearest star. Magnetic solar activity, the total radiative output from the Sun, and the Earth's mean global surface temperature all vary with the 11-year sunspot cycle in which the total number of sunspots varies from a maximum to a minimum and back to a maximum again in about 11 years. The terrestrial magnetic field hollows out a protective magnetic cavity, called the magnetosphere, within the solar wind. This protection is incomplete, however, so the Sun feeds an unseen world of high-speed particles and magnetic fields that encircle the Earth in space. These particles endanger spacecraft and astronauts, and also produce terrestrial aurorae. An international flotilla of spacecraft is now sampling the weak points in this magnetic defense. Similar spacecraft have also discovered a new radiation belt, in addition to the familiar Van Allen belts, except fed by interstellar ions instead of electrons and protons from the Sun.     

太阳耀斑引起的磁扰的多因子回归分析

利用多元逐步回归方法分析了太阳耀斑的日面经纬度、面积,持续时间、地球的日面纬度、地磁轴与日地连线的夹角和地磁扰动的关系。结果表明这6个因子对磁扰均有不同程度的影响,由太阳耀斑引起的地磁扰动除与耀斑的特征有关外,还受地球空间位置的影响。     

Equation for the field lines of an axisymmetric magnetic multipole

Summary. An exact equation is derived for the magnetic field lines of the general axisymmetric magnetic multipole of arbitrary degree ( n ). This new result has important applications in studies of the possible nature of solarterrestrial physics during geomagnetic polarity reversals. In the limiting case of a magnetic dipole ( n=1 ), the equation for the magnetic field lines of the general axisymmetric magnetic multipole simplifies correctly to the well-known dipolar form, which is used extensively in geomagnetism, magnetospheric physics and cosmic-ray physics as a first-order approximation to the actual configuration of the geomagnetic field.
It is also shown theoretically that suites of similar magnetic field lines of the general axisymmetric multipole attain their maximum radial distances from the origin on a set of circular conical surfaces, with coincident vertices at the centre of the Earth; this set includes the equatorial plane if the degree ( n ) of the multipole is odd. The magnetic field is horizontal everywhere on all these surfaces.
Palaeomagnetic studies have suggested that during some polarity reversals the magnetic field in the inner magnetosphere can be represented approximately either by a single, non-dipolar, low-degree (2 < n < 4), axisymmetric magnetic multipole or by a linear combination of such multipoles. In this situation, the equation for the field lines of an axisymmetric magnetic multipole of low degree (2 < n < 4) would be as fundamental to a proper understanding of magnetospheric, ionospheric and cosmic-ray physics during polarity reversals as is the equation for dipolar field lines in the case of the contemporary geomagnetic field.     

地磁数字与模拟观测资料对比分析

“九五”地震前兆数字化台站改造后，数字化的地磁观测仪器在全国各地磁台站推广应用已有两年多时间，两年来，数字化观测仪器和模拟记录仪器在武汉台一直进行并行观测工作，其观测资料稳定可靠。本文通过GM-3磁通门磁力仪与其它仪器进行数字和模拟观测资料的时均值、日均值、月均值、年均值对比分析。分析结果表明数字观测资料优于模拟观测资料，数字观测仪器完全可以取代模拟观测仪器。     

昌黎地磁台地磁变化异常初探

根据磁暴报告，得出昌黎地磁台与同一纬度各台垂直分量△Z的最大幅度差值从几nT到60多nT的差异，初步探讨了昌黎地磁台及其地域地磁变化异常现象。     

Microwave palaeointensity from the R3–N3 geomagnetic field reversal

The microwave palaeointensity technique has been used to determine palaeointensity during the R3–N3 geomagnetic field reversal, using lavas from the Esja region of southwestern Iceland. The resulting intensity determinations have been compared to two previous studies which used the Shaw and Thellier techniques. Both reported low field intensities during the reversal except for four flows that produced high values (20.4–36.8 μT) using the Shaw technique compared to a single maximum intermediate value of 15.9 μT using the Thellier method. In this paper, an average microwave transitional palaeointensity of 6.95 ± 2.07 μT is found for samples used in the Shaw technique study, and of 7.80 ± 1.61 μT for samples used in the Thellier study, demonstrating that there is no evidence for strong fields during this reversal.