Material ejection

This paper reviews the major discussions and conclusions of the Flares 22 Workshop concerning the physical processes involved in mass ejecta events, with an emphasis on large-scale phenomena, especially Coronal Mass Ejections (CMEs). New insights have been gained from recent data obtained from the SMM andYohkoh spacecraft and from several new ground-based radio and optical instruments, as well as from theoretical advances concerning the origins, driving mechanisms and long-term evolution of CMEs.Report of Team 5, Flares 22 Workshop, Ottawa, May 25–28, 1993.     

Coronal index of solar activity: Years 1939–1963

A coronal index of solar activity (CI), based upon the total irradiance of the coronal 530.3 nm green line, has been constructed for the period 1939–1963 from observations at five stations worldwide. The monthly average CI exhibits a cyclic pattern with time, with succesive peaks monotonically increasing since solar cycle 18. Potential uses of the CI are discussed.     

软伽玛射线再暴体（SGRs）研究进展

对SGRs的主要观测特征－－在软伽玛射线波段的重复爆发及持久性的周期的X射线辐射－－进行了回顾，介绍了SGRs的一些理论模型，其中磁星（具有甚强磁场的中子星）模型较合理地解释了现有的观测事实。     

Flares of radio type II and coronal emission in the course of cycle No 20

The butterfly diagram was constructed for the coronal emission of Fe XIV line (530.3 nm) in the course of cycle 1965–1976 complemented with the positions of the source flares with coronal shock waves.     

山东近百年降水的层次结构及趋势诊断

本文采用子波变换的方法分析了山东烟台、济南、青岛近百年降水距平序列,结果表明：气候系统高层次（时间尺度大）的多（少）雨期是由若干中低层次的多雨期或少雨期组成,东部沿海地区的烟台、青岛气候层次为7,降水变化以准70年周期振荡显著,中西部地区的济南气候层次为6,以准11年周期振荡最为显著。在百年以上尺度上,我省未来20年内为降水多雨期或平水期,但还存在中小尺度的降水偏多偏少阶段,2000年以前降水以偏少为主。     

Time profiles of solar irradiance dips

ACRIM data have been analyzed to study the time profiles of simple irradiance dips caused by single active regions. Comparison of the average characteristics of the dips appearing in the minimum and maximum of the solar cycle shows that there are no significant differences. In both periods we disclosed the facular irradiance excess in the profile wings having typical duration of two to three days and an amplitude of about 20% of the dip amplitude. The profiles were asymmetric, with a stronger and longer excess in the trailing wing. We determined an average profile which was attributed to an idealized active region, and we calculated the luminosity perturbation caused by it. Excess radiation in the wings of the profile compensates about 1/3 of the deficit in the dip. In the most simple case from our sample we compared the profile based on ACRIM measurements and the proxy profile estimated using sunspot and plage areas published in Solar Geophysical Data catalogues. The comparison indicates that the facular excess was compensating instantaneously about 2/3 of the luminosity deficit caused by sunspots.     

中国对虾(Penaeus chinensis)肝胰腺上皮细胞质中杆状病毒增殖的电镜观察

对中国对虾肝胰腺上皮细胞进行透射电镜观察。指出：对虾杆状病毒可在肝胰腺上皮细胞的胞质内增殖，与以细胞核内形成包涵体为特征的增殖方式明显不同。溶酶体在增殖过程中内吞濒临解体的线粒体和病原体，利用线粒体内嵴提供的能量，有规律地组装成杆状病毒的包涵体。这一结果为探讨对虾暴发大面积死亡的病因分析提供了新的途径。     

基于网格编码调制(TCM)技术的水声通信系统及DSP实现

阐述了网格编码调制(TCM)的原理及其在水声通信中的应用。采用TI公司的高性能DSP芯片TMS320C542实现了一个可以进行字符传输的水下无线通信系统。试验结果表明，网格编码调制技术能够使水下无线通信系统的性能得到明显改善。     

中国对虾(Penaeus chinensis)病害爆发流行期间杆状病毒亚微形态的电镜观察

对１９９４～１９９５年中国对虾病害爆发期间病虾肝胰脏、鳃、胃及肠组织进 行了透射电镜观察。结果表明，多亚群杆状病毒感染是病害发生的主要原因。杆状 病毒以无包涵体１００～１３０ｎｍ×５００～５２０ｎｍ、１１０～１３０ｎｍ×３００～３３０ｎｍ及有包涵 体的 １００～１３０×３００～３３０ｎｍ ３种形态存在。     

Ignition of MHD shocks associated with solar flares

We have selected single frequency recordings of 28 high-frequency type II bursts characterized by a starting frequency greater than 237 MHz to estimate as accurately as possible the launch-time of the flare-associated MHD shocks. We established the time associations between metric type II burst onsets and the time characteristics of the microwave and X-ray fluxes of the associated flares. The associated flares were impulsive events with rise times most often about 1 min in the hard X-ray range and 1–2 min in the microwave wavelength range. The majority of the type II bursts from our sample started about 1 min after the maximum of the microwave burst. Launch times of MHD shocks producing type II bursts were obtained using the 10 × Saito coronal model and shock velocities estimated from burst characteristics at different frequencies. Back-extrapolations of type II recordings indicate that MHD shocks are launched in the time interval prior to the maximum of the first peak in the associated microwave burst, most probably at the beginning of the rapid increase of the microwave burst.