我国雷暴活动对太阳耀斑响应的东西不对称性

本文研究了１９７１—１９８０年间发生在日面东部的１６４个和西部的１３２个２级以上耀斑对我国１８５个气象站上空雷暴活动的影响．结果表明，日面东部耀斑爆发后雷暴活动减弱且通过优于０．１的置信度检验测站数远多于日面西部耀斑，而日面西部耀斑爆发后雷暴活动增强，通过优于０．１的置信度检验测站数远多于日面东部耀斑．这种与地磁活动和日球扰动相似的雷暴活动对太阳耀斑响应的东西不对称性，可能借助于大气电环境并通过行星际磁场和磁层，将太阳和对流层的确耦合起来了．     

太阳NOAA6891活动区磁中性线的分析

太阳活动高产区NOAA6891是一个岛型δ黑子，它有5条中性线，表现出不同的性质．其中第3条的横场比较弱，但是由于有剪切，所以有耀斑活动．而第2条中性线的横场较大，剪切得非常厉害，所以在这个区域产生了大量的耀斑，包括2个白光耀斑．正因为如此，所以要对磁场作三维分析，其中用磁场拓扑界面来分析是一种好的途径．     

Fine structure of microwave emission in the 25 August 1999 event and its association with the magnetic field fine structure

A study is made of the initial stage of the 25 August 1999, event using high time-resolution microwave observations, as well as the data from the Siberian Solar Radio Telescope and Yohkoh/SXT/HXT. Microwave emission revealed fine structures with a typical time scale of about 1 s with a frequency drift 1 GHz/s, and structures with a typical time scale of less than 0.1 s with a frequency drift 10 GHz/s. Emission bands with a slower frequency drift are generated by energetic electrons subjected to the cyclotron resonance condition. This slower frequency drift is a consequence of a change in plasma density caused by the coalescence of magnetic structures with a typical size of the order of 10⁸ cm, while the emission with a faster drift is generated by beams of energetic electrons generating Cherenkov resonance emission. The energetic electron beams are produced as a result of the interaction of magnetic structures 10⁶–10⁷ cm in size.     

高炮、火箭和飞机催化扩散规律和作业设计的研究

文章基于扩散计算的解析解,提出了针对高炮、火箭和飞机等不同催化方式的点源、多线源和移动点源的数值计算方案,分别研究了不同催化方式催化剂扩散规律和有效范围,并利用卫星捕获的一次飞机播云实例检验了计算方案,同时研究了实现目标区充分催化的作业设计等问题。主要结论有:高炮做为点源催化,单个高炮作业,达到有效催化浓度的范围半径约只有0.5 km,应当采用多炮弹密集作业,比较有利于浓度和催化范围的维持,提高炮弹成核率能够很大程度地提高高炮作业效果;火箭和飞机作为线源催化,1 h内达到有效催化浓度的宽度分别为7和6.6 km,此宽度可作为多线播撒作业飞行间距设计的参考依据;飞机单线播撒达不到充分催化的要求,而耕作式播撒,在风速作用下,扩散区域会分散或重叠。根据风速大小设计的"8"字形来回播撒飞行路线,可使目标区得到充分播撒。在扩散计算方案研究基础上研发的各类催化扩散计算和作业设计软件系统,可方便准确地计算飞机、高炮和火箭实际作业时催化剂在云中扩散的范围、浓度及其随时间的演变,并可针对不同目标区进行充分播撒催化的作业设计,结果直观简明,为催化扩散计算的实际业务应用和作业设计提供了帮助。     

2013年5月强太阳耀斑期间横县电离层特征的分析

通过对2013年5月4次强太阳耀斑爆发期间横县电离层测高仪的电离图和SAO数据进行分析,结果表明：（1）在5月13-15日4次X级的强耀斑过程中,其中有3次电离图上出现了0.5-2小时的描迹线消失过程。（2）每一次描迹消失的起始时间与太阳耀斑爆发的起始时间存在一定的滞后关系,一般在太阳耀斑爆发5-20分钟之后,电离图描迹线才会开始消失,而当耀斑事件停止时,描迹线恢复也会相应的滞后。（3）横县上空的电离层在当地时间上午时段的吸收现象较晚间时段的明显。     

Measurement of 129I in ferromanganese crust with AMS

In the present study,the analytical method for 129iodine(129I) in ferromanganese crusts is developed and129iodine/127iodine(129I/127I) ratio in ferromanganese crusts is measured by the accelerator mass spectrometry(AMS).The developed method is applied to analyze 129I/127 I ratio in two ferromanganese crusts MP5D44 and CXD08-1 collected from the Mid-Pacific Ocean.The results show that 129I/127 I ratio in MP5D44 and CXD08-1crusts varies from 7×10–14 to 1.27×10–12,with the lowest value falling on the detection limit level of AMS reported by previous literatures.For the depth distribution of 129I/127 I,it is found that both MP5D44 and CXD08-1 crusts have two growth generations,and the 129I/127 I profiles in two generations all displayed an approximate exponential decay.According to the 129I/127 I ratio,the generate age of bottom layer of MP5D44 and CXD08-1 was estimated to be 54.77 and 69.69 Ma,respectively.     

10—11月海南省瓜菜苗期湿涝风险评估与区划

为了评估海南省冬种瓜菜苗期生长阶段容易遭受的湿涝灾害,基于1998—2011年海南省18个气象站气象资料、各市县西瓜、豇豆、辣椒、丝瓜4种冬种瓜菜产量及苗期湿涝灾情资料,以降水量、降水日数等因子建立主成分分析综合指标,通过灾情反演构建苗期湿涝致灾等级指标,结合孕灾、灾损和防灾能力进行瓜菜苗期湿涝灾害综合风险分析与区划。结果表明:瓜菜苗期湿涝危险性从西南至东北增加,轻度与重度湿涝风险概率分布趋势相反,苗期湿涝孕灾敏感性从中西部山区向沿海和平原地区增加,瓜菜苗期湿涝灾损风险和防灾能力分布存在差异,且不同瓜菜差异明显;4种瓜菜苗期湿涝综合风险总体分布趋势一致,从西南至东北地区风险等级加重,降水、地势、土地等因素综合导致东部和北部部分地区苗期湿涝的风险高。     

The importance of source positions during radio fine structure observations

The measurement of positions and sizes of radio sources in the observations of the fine structure of solar radio bursts is a determining factor for the selection of the radio emission mechanism. The identical parameters describing the radio sources for zebra structures（ZSs） and fiber bursts confirm there is a common mechanism for both structures. It is very important to measure the size of the source in the corona to determine if it is distributed along the height or if it is point-like. In both models of ZSs（the double plasma resonance（DPR） and the whistler model） the source must be distributed along the height, but by contrast to the stationary source in the DPR model, in the whistler model the source should be moving. Moreover, the direction of the space drift of the radio source must correlate with the frequency drift of stripes in the dynamic spectrum. Some models of ZSs require a local source, for example,the models based on the Bernstein modes, or on explosive instability. The selection of the radio emission mechanism for fast broadband pulsations with millisecond duration also depends on the parameters of their radio sources.     

地球电场与地球磁场的形成机理

为探讨地球磁场的形成机理,应用经典电磁理论以微分的思维方式建立起三种自激发电机模型,用球形自激发电机模型简明地描述地球磁场的形成和分布;从分析地轴参考系中相对于自转地球静止的电荷间洛仑兹力的特点以及地球上的电荷在地球电场和地球磁场作用下的漂移规律,阐述中心磁场的形成及反转机理;分析电荷相对于地球的漂移以阐述偏磁场的形成.理论分析表明:地球上每一点的磁场都可以看成是由该点的几个分磁场叠加而成;地球具有自身的电场;地球电场与地球磁场同时产生、同时变化,且都源自于地球的自转和地球上正负电荷的非对等分布.     

THE STUDY OF HIGH EFFICIENT AgI PYROTECHNICS AND THEIR NUCLEATING PROPERTIES

Two kinds of high efficient Agl pyrotechnics BR-88-5 and BR-91-Y have been developed.The tests in the cloudchamber show that the AgI ice nucleating effectiveness can reach up to 10~(15)/g,and the BR-91-Y has even higher icenucleating rate.Two kinds of foreign AgI pyrotechnics have been made according to the given formulations and alsotested in the cloud chamber for comparison.X-ray diffraction analysis for the aerosols produced by burning BR-91-Yshows that AgI in acrosols still retains the hexagonal crystal form and the lattice parameters are smaller than those ofpure AgI and other AgI composite nuclei,and closer to ice.Combining with the other tests,the reasons for the high effi-ciency of BR-91-Y have been discussed.