重力异常垂向一阶导数的一种简便算法

利用拉格朗日插值导出了重力异常垂向一阶导数的计算公式，给出了地面以及地面之上不同高度的求导系数。该公式可以计算地面上的重力垂向一阶导数，还可以直接计算地面之上任意高度上的垂向一阶导数。鉴于该公式除系数不同外，与上延公式完全相同，因此，程序设计尤为简单。使用本公式对模型数据和实际资料进行了处理，证明了本算法的实用性。     

潮流沙脊的水力学问题探讨

借用河流水力学顺直河道中有两个次生横向环流的假说来解释潮流沙脊的成因，水槽实验和实际观察也支持了这一观点．正是这一次生的纵轴横向环流（即螺旋流）将泥沙从沟槽带向脊顶，建造了大致与潮流方向平行的潮流沙脊．根据底质粒度成份和分布特点．可分为粗底质沙脊和细底质沙脊两类．前者组成物质偏粗，底质分布为脊细槽粗，后者组成物质偏细，底质分布为脊粗槽细．这是因为影响颗粒起动流速的主导因素不同，前者以重力为主，后者以颗粒间粘结力为主．它们都反映沟槽中流速大于脊顶处流速．     

山东省大中型水库水化学性状研究──几种主要水化因子的变化及其在评价水库鱼产力中的作用

本文通过对山东省３８座代表性大、中型水库总氮（ＴＮ）、总磷（ＴＰ）、化学耗氧量、硬度及电导率（λ）五种主要水化因子连续两年（１９８９～１９９０）的调查与研究，探讨了水化因子与水库鱼产力的关系。用反映鲢、鳙生长状况的综合生长指数（ＧＩ）作为水库鱼产力的指标。它与水化因子相关分析表明，总磷是山东省３８座水库鱼产力的主要影响因子。提出ＧＩ与总磷、总氮及电导率等水化因子的逐步回归方程关系非常显著。证明利用水化因子作为水库鱼产力的评价指标是可行的。并指出：同一水库的相同水化因子存在年间差异，其主要原因在于降雨量和水库进水量的不同，鉴于此．同一水库鱼产力也存在年间差异。     

Chemistry of marine resources-ⅩⅨ. The molecule design and synthesis of crow-link type alkyd resin and its enrichment behaviour for potassium ion in sea water

This paper first presents the molecule design and synthesis of crown-link type alkyd resin,and its enrichment behaviour for potassium ion in low concentration solution and sea water.On the basis of some theory concepts of Host-Guest chemistry developed in recent years,we have designed and synthesized a new polymer enrichment agent of crow-link resin for potassiumion,i.e.,polymacrocyclic ether bislactone of diethylene glycolpyromyllitic acid(briefly called crown-link type alkyd resin or PBL resin).The yield was about 97.4%,almost quantitatively.     

2021年10月山西一次罕见持续性强降水过程物理机制分析

利用气象观测资料、NCEP/NCAR 1°×1°再分析资料以及GDAS资料,对2021年10月2-7日山西持续性强降水天气过程进行分析。结果表明：稳定的乌拉尔山低槽后部冷空气扩散,中纬度短波槽东移,与副热带高压外围西南暖湿气流持续交汇,同时高低空急流耦合形成强烈上升运动,低层切变线和地面辐合线稳定维持,及低层水汽不断输送并形成辐合,为持续性强降水的发生发展提供有利动力和水汽条件。此次强降水过程分为对流性降水和稳定性降水2个阶段,2阶段水汽输送通道的源地、路径、高度均有明显差异,但水汽输送贡献率均以对流层中低层山西南侧的水汽输送占主导地位。降水开始前,对流层中上层存在对称不稳定,大气可降水量明显跃增;对流性降水阶段,干空气不断入侵,对流不稳定快速建立与释放,对流层中低层水汽辐合区与强上升气流配合,导致山西出现强对流天气。地形的阻挡、抬升及地形收缩作用,对局地极端强降水具有增幅作用。     

Studies on post-flare loop prominence of 1981 April 27

By use of the H observations of the Astrophysical Observatory in Catania, Italy and the Purple Mountain Observatory in Nanking, China as well as hard X-ray and gamma-ray burst data from the Solar Maximum Mission (SMM) Gamma-Ray Spectrometer (GRS), a major eruptive loop prominence was studied during the limb solar flare event of 1981 April 27.Our preliminary analysis shows that there seems to exist a second abrupt energy release for this event, almost 20 min after the end of the impulsive phase of the flare. This energy release is probably associated with the rapidity in upward motion or activation of the loop prominence.A possible candidate for such a process could be the reconnection of the old magnetic field with a newly emerging magnetic field.A theoretical gross estimate for the energy release and particle acceleration has also been made in this work. It appears that the proposed model for charged particle acceleration is very efficient.     

滇西地区地壳上地幔电性结构与地壳构造活动的关系

本文根据滇西地区18个大地电磁测深点资料的数据处理和分析结果,对测区深部导电率在纵、横向上的变化特征进行了研究。结果表明:滇西地区深部电性为多层结构,大致可分四至五个电性结构层;深部电性结构横向变化大,明显受区域构造控制;该区上部地壳内普遍存在低阻层;上地幔高导层明显存在两个隆起区,一个以剑川—鹤庆为中心呈北北西向展布的隆起区,另一个以腾冲—潞西为轴呈南北向展布的隆起区。 本文还讨论了地壳上地幔电性结构与大地构造的关系,滇西北裂陷区盆地的形成,以及该区地震活动与深部构造的关系     

The light curved in the CM field

In this paper we introduce the CM field in Sections 2 and 3 based on the paper by Wang and Peng (1985), and calculate the light curved in the CM field in Section 4. The result shows thatP makes _CM larger than _C at , and smaller at . Under a special circumstance which source, CM lens, and observer are in the same line, if we get | ₀₌₀ , and | _=/2 , we can determine theP(M) andQ(M) of the CM lens,M is the mass of the CM lens.     

早第三纪济阳湖盆的形成和演变

在构造和气候的综合作用下,本区在早第三纪成为一个大型裂谷湖盆,并在沙四、沙三和沙一期因受古太平洋海泛影响而具有"近海"湖盆的特征,其演变经历了初始形成-强烈扩张-晚期扩张-收缩干涸四个阶段,构成一个完整的湖侵-湖退旋回和湖泊早期形成-中期扩张-晚期收缩三个亚旋回。     

Flows around sunspots and pores

We report on three sequences of high-resolution white-light and magnetogram observations obtained in the summer of 1989. The duration of sub-arcsecond seeing was three to four hours on each day. Study of the white-light and magnetogram data yields the following results:

1. For all but one of the sunspots we have observed, both dark fibrils and bright grains in the inner part of the penumbra of sunspots move toward the umbra with a speed of about 0.5 km s^-1. In the outer part of the penumbra, movement is away from the umbra. The one exception is a newly formed spot, which has inflow only in its penumbra.
2. Granular flows converge toward almost every pore, even before its formation. Pores are observed to form by the concentration of magnetic flux already existing in the photosphere. The pores (or small sunspots), in turn, then move and concentrate to form bigger sunspot.
3. We followed an emerging flux region (EFR) from 29 to 31 July, 1989 that was composed of a large number of bipoles with magnetic polarities mixed over a large area in the first day of its birth. As time went on, polarities sorted out: the leading polarity elements moved in one direction; the following, the opposite. During the process a large number of cancellations occurred, with some sub-flares and surges observed simultaneously. After about 24 hours, the positive and negative fluxes were essentially separated.
4. We find two kinds of photospheric dark alignments in the region of new flux emergence: (a) alignments connecting two poles of opposite magnetic polarity form the tops of rising flux tubes; (b) alignments corresponding to the magnetic flux of one polarity, which we call elongated pores.