切向结构永磁同步电机中磁钢厚度对性能的影响

提出了切向结构永磁同步电机中磁钢厚度的约束条件;依据电机学理论并结合有限元计算方法,研究了气隙长度恒定时不同极对数下气隙磁密、每极磁通与磁钢厚度的关系,探讨了磁钢厚度对电机的过载能力、铁耗等性能的影响;在气隙长度发生变化时,为了保证漏磁大小不变,讨论了气隙与非导磁衬套厚度、磁钢厚度的关系。并指出:(1)气隙恒定时,随着磁钢厚度的增加,不同极对数时磁钢体积增大所提供的磁势对每极磁通的影响有所不同;铁耗和过载能力随磁钢厚度的增加而增大。(2)气隙增大时,为了保证气隙磁密和漏磁不变,必须增加非导磁衬套的厚度。(3)极对数增加时,减小磁钢厚度能提高电机的性价比。     

车载中频高速同步发电机设计

对车载中频高速同步发电机设计思路和设计特点进行阐述。根据设计思路和设计特点制造了试验样机,在制造过程中着重对磁极线圈的绑扎与固定、三相旋转整流器的内部结构做了改进。进行了电机性能的试验分析,对采取的技术措施进行验证,验证了设计方法的有效性。这为同类电机设计提供了参考。     

Energy input for explosive events in the transition zone

It is suggested that the energy input for explosive events in the transition zone comes from precipitating ions, typically of energies of a few×10² keV/nucleon, accelerated in the high corona. The energetics of the process are discussed, together with implications for coronal heating.     

Working group 3: Coronal streamers

The working group on coronal streamers convened on the first day of the 2nd SOHO Workshop, which took place in Marciana Marina, Isola d'Elba, 27 September –1 October 1993. Recent progress in streamer observational techniques and theoretical modeling was reported. The contribution of streamers to the mass and energy supply for the solar wind was discussed. Moreover, the importance of thin electric current sheets for determining both the gross dynamical properties of streamers and the fine-scale filamentary structure within streamers, was strongly emphasized. Potential advances to our understanding of these areas of coronal physics that could be made by the contingent of instruments aboard SOHO were pointed out.     

质子耀斑活动区的再现规律

质子耀斑活动区再现规律的研究结果表明，日面上存在着经度方向漂移式的“活火山”，即质子活动复活体，“活火山”定期地复活，并爆发质子耀斑。其复活长周期为８－１１．６年，与活动周１１年周期基本一致；短周期为１．２６年，与活动周峰年时间宽度一致。在２２周峰年中，日面南北半球上各有一个强质子活动复活体，它们爆发值流量≥１００ｐｆｕ和≥１０００ｐｆｕ的质子耀斑各占周期同类耀斑总数的７０．７％和８３．３％。     

无人机螺旋桨实验天平的研制

螺旋桨实验是一种非常规实验 ,其特点决定了螺旋桨天平的特殊性。为了探索新的扭矩测量方法 ,准确研究螺旋桨的性能 ,设计了螺旋桨实验专用天平。该天平是同步旋转应变天平 ,实验中天平随螺旋桨高速旋转。天平设计要保证质量分布均匀 ,采用特制滑环引出电信号 ,并且天平后端用支架支撑以减小振动。该天平较一般固定式天平复杂 ,但更合理地解决了扭矩测量问题。实验结果表明 ,天平总体方案正确 ,设计合理 ,测量精度高 ,有效解决了小型螺旋桨实验问题     

卫生捕获太阳的新方法

对卫星入轨后捕获太阳的方法进行了研究,并对一种有效的控制规律进行了分析计算,最后对卫星的运动过程进行了仿真验证。     

Chromospheric line emission in seismically active flares

Some flares are known to drive seismic transients into the solar interior. The effects of these seismic transients are seen in helioseismic observations of the Sun’s surface thousands of km from their sources in the hour succeeding the impulsive phase of the flare. Energetic particles impinging from the corona into the chromosphere are known to drive strong, downward-propagating shocks in active region chromospheres during the impulsive phases of flares. H observations have served as an important diagnostic of these shocks, showing intense emission with characteristic transient redshifts. In most flares no detectable transients penetrate beneath the active region photosphere. In those that do, there is a strong correlation between compact white-light emission and the signature of seismic emission. This study introduces the first known H observations of acoustically active flares, centered in the core of the line. The morphology of line-core emission H in the impulsive phase of the flare is similar to that of co-spatial line-core emission in NaD₁, encompassing the site of seismic emission but more extended. The latter shows a compact red shift in the region of seismic emission, but a similar feature is known to appear in a conjugate magnetic footpoint from which no seismic emission emanates. Radiative MHD modelling based on the profiles of chromospheric line emission during the impulsive phases of flares can contribute significantly to our understanding of the mechanics of flare acoustic emission penetrating into the solar interior and the conditions under which it occurs.     

IS-95 CDMA前向同步信道仿真

分别对IS-95码分多址标准和SystemView软件进行了介绍,概述了IS-95前向同步信道的基本特点和性能参数,给出了采用SystemView软件仿真IS-95码分多址标准前向同步信道的方法和仿真结果。     

Quasi-biennial oscillations in the cross-correlation of properties of macrospicules

Jets, whatever small (e.g. spicules) or large (e.g. macrospicules) their size, may play a key role in momentum and energy transport from photosphere to chromosphere and at least to the low corona. Here, we investigate the properties of abundant, large-scale dynamic jets observable in the solar atmosphere: the macrospicules (MS). These jets are observationally more distinct phenomena than their little, and perhaps more ubiquitous, cousins, the spicules. Investigation of long-term variation of the properties of macrospicules may help to a better understanding of their underlying physics of generation and role in coronal heating. Taking advantage of the high temporal and spatial resolution of the Solar Dynamics Observatory, a new dataset, with several hundreds of macrospicules, was constructed encompassing a period of observations over six years. Here, we analyse the measured properties and relations between these properties of macrospicules as function of time during the observed time interval. We found that cross-correlations of several of these macrospicule properties display a strong oscillatory pattern. Next, wavelet analysis is used to provide more detailed information about the temporal behaviour of the various properties of MS. For coronal hole macrospicules, a significant peak is found at around 2-year period. This peak also exists partially or is shifted to longer period, in the case of quiet Sun macrospicules. These observed findings may be rooted in the underlying mechanism generating the solar magnetic field, i.e. the global solar dynamo.