黑子磁流体静力学的一个模型

本文对Ｏｓｈｅｒｏｖｉｃｈ的黑子返回磁通量模型作了适当的修改，使用黑子中心作为边界条件，用五种观测结果，导出了理论模型所需的五个主要参量，用半经验方法求得了黑子静力学模型的磁场、压力和温度等物理量．将此模型应用于一个中等大小的圆形对称黑子，可得到一个特解，结果发现我们的模型既能满足黑子的磁性质，同时又能满足合理的热力学量分布．     

太阳黑子相对数与人类疾病关系的初步分析

从日地关系的角度出发,探讨太阳活动对人类疾病有何影响。本文根据南京市传染病医院的资料,对每种疾病人数的相对比率与太阳黑子相对数对应作图比较,并求出其相关系数。我们的初步结果表明:伤寒和猩红热的发病率与太阳活动11年周期变化一致,它们在同年达到极大值,其它的不明确。     

景观单元评价方法

本文通过对瓜达卢皮山国家公圆的分区和评价,提出了一种对土地系统和景观单元进行划分的方法。划分土地系统和景观单元,以许多相关因素作为基础。给一些小的区域下定义,然后再将这些小区域合并成大区域。     

南平塔下-果园一带变质杂岩的变形、变质史及地层工作方法讨论

一、概述测区位于福建省南平市东2～3.5公里的闽江北滩,面积约3平方公里(图1)。在省区测队(1977)主编1:50万省地质图上,测区地层划归前震旦系建瓯群大岭组(An Zzdl)。     

Magnetic Field Strengths and Structures from Radio Observations of Solar Active Regions

Radio observations of some active regions (ARs) obtained with the Nobeyama radioheliograph at λ=1.76cm are used for estimating the magnetic field strength in the upper chromosphere, based on thermal bremsstrahlung. The results are compared with the magnetic field strength in the photosphere from observations with the Solar Magnetic Field Telescope (SMFT) at Huairou Solar Observing Station of Beijing Astronomical Observatory. The difference in the magnetic field strength between the two layers seems reasonable. The solar radio maps of active regions obtained with the Nobeyama radioheliograph, both in total intensity (I-map) and in circular polarizations (V-map), are compared with the optical magnetograms obtained with the SMFT. The comparison between the radio map in circular polarization and the longitudinal photospheric magnetogram of a plage region suggest that the radio map in circular polarization is a kind of magnetogram of the upper chromosphere. The comparison of the radio map in total intensity with the photospheric vector magnetogram of an AR shows that the radio map in total intensity gives indications of magnetic loops in the corona, thus we have a method of defining the coronal magnetic structure from the radio I-maps at λ=1.76 cm. Analysing the I-maps, we identified three components: (a) a compact bright source; (b) a narrow elongated structure connecting two main magnetic islands of opposite polarities (observed in both the optical and radio magnetograms); (c) a wide, diffuse, weak component that corresponds to a wide structure in the solar active region which shows in most cases an S or a reversed S contour, which is probably due to the differential rotation of the Sun. The last two components suggest coronal loops on different spatial scales above the neutral line of the longitudinal photospheric magnetic field.