冷空气引起的飞船主着陆场区偏北大风的特征分析及预报

分析了飞船主着陆场区1981—1999年1—4月和9—12月因冷空气而产生的偏北大风的过程中气候概况及其天气特征。通过分析发现:主着陆场区因冷空气引起的偏北大风以春季最频繁,秋、冬季最稀少;一天当中偏北大风以午后出现频率最大,午夜出现频率最少;对于不同季节的气压和温度,春、秋两季变化剧烈,冬季相对较小;在大风出现前24小时,主着陆场区的欧亚中高纬度大气环流以两槽一脊型、一槽一脊型、贝湖低压型为主;冷空气入侵前24小时,欧亚天气图上主着陆场区上游低层850hPa中高纬度有明显的冷中心,地面图场区上游冷高压中心的分布主要有3个区域:贝加尔湖西南至新疆、贝加尔湖到内蒙中北部、贝加尔湖西北部。大风前24小时在35～45°N、100～115°E等压线密集,等压线一般都在4根以上。     

山东乳山英格庄金矿床地质特征及成因浅析

英格庄金矿为胶东牟平-乳山成矿带上的一个中型金矿床。该矿床矿体严格受金牛山断裂带控制,呈脉状、透镜状和囊状平行斜列式产出;矿体平均厚1．58～1．98m,平均品位3．96×10^-6～4．77×10^-6。矿石类型主要为黄铁矿石英脉型;矿石中金属矿物主要为银金矿、自然金、黄铁矿等。围岩蚀变包括绢云母化、硅化、绿泥石化、黄铁矿化等。研究表明,英格庄金矿床为一中低温热液脉型金矿,属Groves等提出的造山型金矿范畴。     

浅论县（市）级土地利用数据库系统建设

随着经济的迅猛发展,各地土地利用情况多种多样,采用手工管理土地资料更新周期长,综合利用率低,各种查询统计要耗费大量的人力物力,而且统计计算的数据结果精度不高。因此仅仅依靠传统的手工管理模式已经远远不能满足土地管理工作的需要,为保质保量按时完成全国土地利用现状更新调查,加强地籍规范化管理,利用成熟的计算机技术辅助进行土地调查已势在必行。     

胶体磷在河口IX随盐度变化的研究

研究了胶体磷在河口海区随盐度变化的趋势,并将其与颗粒态、真溶解态磷随盐度的变化趋势进行对比,分析胶体态磷在河口的行为与颗粒态磷和真溶解态磷二者的异同.探讨磷在颗粒相,胶体相和真溶液相之间的分配及其与悬浮颗粒物浓度的关系,研究胶体磷在河口海区中的迁移转化作用.研究结果表明,胶体相中总磷、有机磷和活性磷浓度由河端向海端降低,表明陆源输入是其主要来源.胶体有机磷占总磷比例随盐度增加而下降,表明有机磷受胶体去除过程的影响较明显,胶体磷在河口海区的浓度变化趋势及胶体中有机磷和活性磷的比例都与真溶解相接近而与颗粒相差别较大.     

On the propagation of chromospheric condensations in solar flares (II)

We study the evolution of the mass motion velocity in the chromospheric condensation, when it propagates into the deeper atmosphere. The condensation is represented by a shock-like structure. Its momentum equation can be solved after some approximations. The computations are carried out for two cases, i.e., the case that the gas pressure just behind the condensation front is constant and the case that the pressure increase at the top of the condensation is constant. The results show that the duration of the condensation in the second case is considerably longer than that in the first case. The most evident difference of the velocity evolution between the two cases appears in their later phase. A comparison of the results in this paper with the dynamic simulations indicates that the second case may be closer to the real situation.     

Flare-induced signals in polarization measurements during the X2.6 flare on 2005 January 15

Flare-induced signals in polarization measurements which were manifested as apparent polarity reversal in magnetograms have been reported since 1981. We are motivated to further quantify the phenomenon by asking two questions: can we distinguish the flare-induced signals from real magnetic changes during flares, and what we can learn about flare energy release from the flare-induced signals? We select the X2.6 flare that occurred on 2005 January 15, for further study. The flare took place in NOAA active re-gion (AR) 10720 at approximately the central meridian, which makes the interpretation of the vector magnetograms less ambiguous. We have identified that flare-induced signals during this flare appeared in six zones. The zones are located within an average distance of 5 Mm from their weight center to the main magnetic neutral line, have an average size of (0.6±0.4)×1017 cm2, duration of 13±4 min, and flux density change of 181±125 G in the area of reversed polarity. The following new facts have been revealed by this study: (1) the flare-induced signal is also seen in the transverse magnetograms but with smaller magnitude, e.g., about 50 G; (2) the flare-induced signal mainly manifests itself as apparent polarity reversal, but the signal starts and ends as a weakening of flux density; (3) The flare-induced signals appear in phase with the peaks of hard X-ray emission as observed by the Ramaty High Energy Solar Spectroscopic lmager (RHESSI), and mostly trace the position of RHESSI hard X-ray footpoint sources. (4) in four zones, it takes place cotemporally with real magnetic changes which persist after the flare. Only for the other two zones does the flux density recover to the pre-flare level immediately after the flare.The physical implications of the flare-induced signal are discussed in view of its relevance to the non-thermal electron precipitation and primary energy release in the flare.     

Environmental dependence of stellar mass,SFR, and SSFR for the Luminous Red Galaxy (LRG) sample of the SDSS DR7

Using the Luminous Red Galaxy (LRG) sample of the Sloan Digital Sky Survey Data Release 7 (SDSS DR7), we investigate the environmental dependence of stellar mass, star formation rate (SFR) and specific star formation rate (SSFR) of LRGs. It is found that stellar mass of LRGs nearly is independent of local environments, and that the environmental dependence of SFR and SSFR in the LRG sample is much weaker than the one in the Main galaxy sample. One possible explanation is that galaxy color and morphology are a pair of galaxy properties most predictive of local environments, while LRGs are a group of galaxies that are likely to be luminous, red and of early types (© 2012 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

土层地震反应传递函数的模拟

探讨了用单一土层模型替换复杂场地求解土层场地传递函数的方法,并用ＳＭＡＲＴ－１台阵地震记录对这一方法的可行性进行了研究和讨论,结果表明,只要选取适当的地震波入射角Ψ和土介质的滞回阻尼比ｄ,简化模型的传递函数与实际传递函数能符合得较好,这一方法可用来近似估计缺少详细土质勘测资料地区的土层地震反应的传递函数。     

论山地研究的层次性

地壳表面演变全过程大体分为三个重要阶段,即环境演化、生态演化和人类社会全球化阶段。首次从这一角度分析山地科学研究的内容,确立了环境山地、生态山地和人文山地研究层次性体系,并提出在全球化进程中,人类宜重视山地层次性研究与开发、山地自然环境和生态资源的协调性发展,使山地成为优势态的人文生态环境。