论中国经济区域的再形成

经济区域空间格局变化是区域经济不断发展的外在化表现，文章从区域、经济区域等基本概念入手，以经济全球化为背景，分析了市场机制作用下中国经济区域再形成过程的态势和外部环境变化，指出随着我国经济体制改革的深入进行，应积极培育合理经济区、建立合理的区际分工体系、培育区域之间合理的竞争态势，以提高我国区域竞争力和国家竞争力。     

21世纪初叶中国治贫反困新思路

21世纪初叶中国的贫困形势是乡村贫困与城市贫困共存，绝对贫困与相对贫困共存，区域性贫困与阶层性贫困共存。文章针对我国反贫困工作中存在的主要问题，提出了建立有效的反贫困治理结构、妥善解决城镇贫困问题、加强国际间合作等对策。     

环洞庭湖区城镇体系发展研究

通过对环洞庭湖区城镇体系发展的历史背景以及现状特征分析，指出其发展过程存在着城市空间格局发展不平衡，产业结构重复严重等问题，在此基础上，提出了相应的对策与发展措施，确保环湖区内城镇体系的持续，快速发展，并最终实现带动区域经济发展的目的。     

陕西凤县金矿类型与金的预富集及找矿方向

陕西凤县地区金矿主要有蚀变岩与石英脉型。地层预富集是金矿形成的物质基础；岩体为金矿形成提供了Au源，而且沿构造蚀变带提供了热源，是Au活化成矿的一个重要条件；多期次热液沿构造破碎带进行交代改造形成蚀变预富集，是金矿成矿的关键。庞家河成矿模式为层预富集＋蚀变预富集＋后期多次热液交代富集成矿；佐家庄成矿模式为岩体（脉）预富集＋构造蚀变预富集＋多种热液叠加成矿。NNW向断裂带是寻找蚀变岩型金矿的主要标志；印支期与华力西期花岗岩－闪长岩带的内外接触带是寻找石英脉型及蚀变岩型金矿的主要构造带；金的预富集带是金矿成矿的有利部位，紧靠商丹大断裂南侧续分布的残余存小岩块旁侧都发现金矿床。     

古吉黑造山带拼接带地球物理特征线

吉黑造山带拼接带的地球物理特征线，在重磁图上为伊通-吉昌-桦甸、贤儒-安图-开山屯一线。它分割了两种截然不同的地球物理场区，与两侧中元古宙-早三叠世不同的地质发育历史相呼应；和石炭-二叠系安哥拉与华夏植物地球区系的界线相一致。这是有别于前人而为更多新的地质资料所支持的新认识。     

长春市地下水开发环境问题研究

本文根据近期地下水动态监测资料，结合地下水赋存的环境水文地质条件，分析论述了长春市由于不合理开发地下水资源而产生地下水水位下降，水量削减、水质污染、地面沉降等环境地质问题，提出了防治对策及建议。     

低氟与大骨节病－－大骨节病防治拾趣四则

该文笔者多年研究大骨节病原始原因的一项新说。即病区外环境低氟。引起体内以低氟为中心的代谢紊乱，从而导致以骨骼系统为主的病变－大骨节病。防治该病，应向体外补氟。药疗这一进补方式故然必然，但最有效又生活化的办法是食疗。食疗又分氟盐防治和饮茶防治两种。而最适用且简便的方法是提倡患区人群适度饮茶，并且应从儿时做起。关于补氟和饮茶等防治大骨节病的实践，笔者已浓缩于下面四则拾趣之中……。     

考虑湿度影响的城市气溶胶夜晚温度效应

本文利用一维非定常模式，研究了城市上空干、湿气溶胶粒子对夜间边界层温度的影响。结果表明，湿气溶胶粒子对低层大气有明显的升温作用，而对中上层大气则起降温作用，同时改变了贴地逆温层结构和边界层稳定度。     

Multifractal scaling of the kinetic energy flux in solar wind turbulence

The geometrical and scaling properties of the energy flux of the turbulent kinetic energy in the solar wind have been studied. Using present experimental technology in solar wind measurements we cannot directly measure the real volumetric dissipation rate, <varepsilon>(t), but are constrained to represent it by its surrogate the energy flux near the dissipation range at the proton gyro scale. There is evidence for the multifractal nature of the so defined dissipation field <varepsilon>(t), a result derived from the scaling exponents of its statistical moments. The generalized dimension D _q has been determined and reveals that the dissipation field has a multifractal structure, which is not compatible with a scale-invariant cascade. The related multifractal spectrum f(<alpha>) has been estimated for the first time for MHD turbulence in the solar wind. Its features resemble those obtained for turbulent fluids and other nonlinear multifractal systems. The generalized dimension D _q can for turbulence in high-speed streams be fitted well by the functional dependence of the p-model with a comparatively large parameter p ₁=0.87, indicating a strongly intermittent multifractal energy cascade. The experimental value for D _p/3 used in the scaling exponent s(p) of the velocity structure function gives an exponent that can describe some of the observations. The scaling exponent <mu> of the autocorrelation function of <varepsilon>(t) has also been directly evaluated, being 0.37. Finally, the mean dissipation rate was determined, which could be used in solar wind heating models.     

An extended structure-function model and its application to the analysis of solar wind intermittency properties

An extended structure-function model is developed by including the new effect in the p-model of Meneveau and Sreenivasan which shows that the averaged energy cascade rate changes with scale, a situation which has been found to prevail in nonfullydeveloped turbulence in the inner solar wind. This model is useful for the small-scale fluctuations in the inner heliosphere, where the turbulence is not fully developed and cannot be explained quantitatively by any of the previous intermittency turbulence models. With two model parameters, the intrinsic index of the energy spectrum <alpha>, and the fragmentation fraction P ₁, the model can fit, for the first time, all the observed scaling exponents of the structure functions, which are calculated for time lags ranging from 81 s to 0.7 h from the Helios solar wind data. From the cases we studied we cannot establish for P ₁ either a clear radial evolution trend, or a solar-wind-speed or stream-structure dependence or a systematic anisotropy for both the flow velocity and magnetic field component fluctuations. Generally, P ₁ has values between 0.7 and 0.8. However, in some cases in low-speed wind P ₁ has somewhat higher values for the magnetic components, especially for the radial component. In high-speed wind, the inferred intrinsic spectral indices (<alpha>) of the velocity and magnetic field components are about equal, while the experimental spectral indices derived from the observed power spectra differ. The magnetic index is somewhat larger than the index of the velocity spectrum. For magnetic fluctuations in both high- and low-speed winds, the intrinsic exponent <alpha> has values which are near 1.5, while the observed spectral exponent has much higher values. In the solar wind with considerable density fluctuations near the interplanetary current sheet near 1 AU, it is found that P ₁ has a comparatively high value of 0.89 for V _x . The impact of these results on the understanding of the nature of solar wind fluctuations is discussed, and the limitations in using structure functions to study intermittency are also described.