超低频计量自动测试系统

充分利用现有的标准仪器,在微机统一控制下,组成一个超低频参数计量的自动测试系统。系统中各台仪器仍保持其独立工作能力。整个计量测试过程,都用软件控制,自动完成,并能对数据自动采集和处理,用汉字打印输出检测结果。     

8802超低频标准相位产生器

８８０２超低频标准相位产生器采用数字技术,用Ｄ／Ａ变换方法产生正弦信号,由单片机控制频率和相位,频率由晶振综合产生,相位可数字预置,频率准确度高至±５×１０￣（－６）,相位准确度高至±０．０００２°。介绍了主要技术指标、工作原理、技术特点和误差分析等。     

一种高准确度超低频电压测试标准——8801超低频电压及失真测试仪

8801超低频电压及失真测试仪是一种采用单片计算机、A/D变换器的采样-计算式仪器,它可以测试超低频信号的周期、电压、失真和谐波等各种参数。电压测试不确定度高达0.02％。文中介绍了主要技术指标、工作原理、技术特点、误差分析等,对软件作了简要说明。     

低频天波远距离传播日、季变化的观测与分析

本文给出了1987年6月至1988年9月间在新多对琉璜岛罗兰-C导航发射台的100kHz低频信号一跳天波“影区”传播的日变化与季变化特性所做观测的基本结果并对其做了分析。通过分析揭示出了我国中纬地区低频天波远距离传播日变化、季变化、幅度跌落效应与干涉效应的产生机制与变化规律;还揭示了我国中纬地区白天低电离层所具有的双层结构特性:在D层下C层的存在以及它们的某些形态特性与季变特性。     

超低频发信天线及其全向等功率辐射技术

介绍了超低频信号的通信特点及其在潜艇通信应用中的地位和概况,研究了提高发信天线辐射效率及全向辐射的超低频对潜通信天线的技术与方法,分析了全向辐射的超低频天线阵方向特性.     

超低频调频标准

所介绍的超低频调频标准在国内处于领先地位,它能提供准确的超低频调频信号,作为调频标准用于超低频调频参数的计量测试。介绍了建立超低频调频标准的目的、应用范围、主要技术参数、基本原理、误差分析、试验结果及其分析和结论。     

高准确度的超低频交流电压表设计

分析了超低频交流电压信号的测量方法,设计了基于采样计算方式的超低频交流电压测量方案。设计了以高速高精度A/D转换器和高性能DSP处理器为核心的超低频交流电压表硬件电路,设计了基于线性插值的非同步采样同步化算法,设计了基于复合梯形求积公式的有效值算法。对所研制的超低频交流电压表进行了量值溯源与校准测试,测试结果表明所研制的超低频交流电压表测量频率下限达到了0.001Hz,测量不确定度优于0.01%。     

基于风云3C卫星观测数据的全球重力波活动特性研究

大气重力波是临近空间中重要的动力学过程之一,并且广泛存在于全球大气层中,研究其全球分布及变化规律,对理解大气动力学具有重要意义。全球卫星导航系统（GNSS）可以通过掩星的方式来获取临近空间大气的温度信息,并且具有全球覆盖、垂直和水平分辨率较高的优点,从而被广泛应用于临近空间大气重力波研究。利用气象卫星风云3号C星（FY-3C）搭载的全球导航卫星掩星接收机（GNOS）的探测数据来反演全球重力波扰动分布,反演得到了2015－2019年这5年间的全球重力波分布,并着重分析了全球重力波的季节变化、年际变化以及长波和短波重力波的全球分布和特征。结果表明,冬夏两季的重力波扰动要强于春秋两季,并且呈现冬季半球强于夏季半球的现象; 同时还发现,重力波扰动的强度随着高度增加而逐渐增强;在20～50 km的高度范围内短波重力波强度大于长波重力波强度。     

一种超低频标准电压和标准相位产生器

该仪器用来产生超低频标准电压和标准相位。它采用数—模变换的方法产生模拟正弦信号,用参考标准直流电压确定输出电压,具有移相输出和参考输出。介绍了仪器的工作原理和所采取的技术措施,进行了误差分折。     

太阳风中低频离子静电孤波

本文给出在太阳风超声速流动条件下,离子静电孤波的传播特性,结果与Helios1,2卫星观测的静电离子噪声做了比较。离子声波扰动的非线性发展使太阳风等离子体呈规则的小尺度起伏,离子声波在马赫锥外传播,因此理论预言密度起伏不沿着太阳风速度方向,而是在横向方向.     

Polarization pattern of low and mid-frequency magnetic pulsations in the polar cap: A comprehensive analysis at Terra Nova Bay (Antarctica)

The polarization pattern of ULF pulsations (f ≈ 1–100 mHz) at Terra Nova Bay (Antarctica, CGM λ ∼ 80°) has been determined for the entire 2003, soon after the solar maximum. A comparison with the results of previous investigations, conducted at the same station close to the solar minimum (1994–96), allows to focus common elements and major differences among different frequency bands which persist through the entire solar cycle. Basically, between f ∼ 1.5 and 5 mHz, the day can be divided into four sectors with alternate polarizations. The local time and latitudinal dependence of the observed pattern can be tentatively interpreted in terms of a latitude of resonant field lines reaching λ ∼ 80° in the noon sector; on the other hand, resonance effects of lower latitude field lines can be clearly identified also far from the noon meridian when the station moves into the deep polar cap. Moreover, in the morning sector the resonance region would extend to lower latitudes than in the evening sector. The proposed profile of the resonant region can interpret also the results obtained at other cusp/auroral stations and appears consistent with that one inferred in the northern hemisphere at smaller latitudes. The resonance region progressively shifts toward lower latitude with increasing frequency; correspondingly, the four-sector pattern progressively disappears at TNB. Above f ∼ 20 mHz, the experimental observations might suggest an additional contribution from Sunward propagating waves, possibly via the magnetotail lobes.     

Study of waves in the magnetotail region with cluster and DSP

The study of the neutral sheet is of fundamental importance in understanding the dynamics of the Earth’s magnetosphere. From the earliest observation of the magnetotail, it has been found that the neutral sheet frequently appears to be in motion due to changing solar wind conditions and geomagnetic activity. Multiple crossings of the neutral sheet by spacecraft have been attributed to a flapping motion of the neutral sheet in the north–south direction, a wavy profile either along the magnetotail or the dawn–dusk direction. Cluster observations have revealed that the flapping motions of the Earth’s magnetotail are of internal origin and that kink-like waves are emitted from the central part of the tail and propagate toward the tail flanks. This flapping motion is shown here to propagate at an angle of ∼45° with x_GSM. A possible assumption that the flapping could be created by a wake travelling away from a fast flow in the current sheet is rejected. Other waves in the magnetotail are found in the ULF range. One conjunction event between Cluster and DoubleStar TC1 is presented where all spacecraft show ULF wave activity at a period of approximately 5 min during fast Earthward flow. These waves are shown to be Kelvin–Helmholtz waves on the boundaries of the flow channel. Calculations show that the conversion of flow energy into magnetic energy through the Kelvin–Helmholtz instability can contribute to a significant part of flow breaking between Cluster and DoubleStar TC1.     

Magnetospheric and ionospheric manifestations of interplanetary foreshocks

The geometry of a typical interplanetary shock front in the vicinity of the Earth’s orbit predicts that the leading edge of the foreshock region comes into contact with the magnetosphere a few hours ahead of geomagnetic sudden impulses (SI). There is reason to believe that the interaction of the magnetosphere with the foreshock leads to magnetic and ionospheric disturbances, which can be detected by ground-based instruments. We searched for specific precursors of SIs in data from the Scandinavian riometer network and in the short period geomagnetic pulsation data from mid-latitude magnetometers. We found that SIs were preceded by the following three features: (1) an increase in riometric absorption, (2) excitation of Pcl magnetic pulsations and (3) a spectral broadening of the Pc3 magnetic pulsations. Our observations may be useful for the study of acceleration processes in the solar wind. These observations are also of potential forecasting interest.     

Ionospheric and geomagnetic Pc5 oscillations as observed by the ionosonde and magnetometer at Sodankylä

The study is based on the data of the rapid-run ionosonde at the Sodankylä Geophysical Observatory at auroral latitude (L?=?5.25) which routinely performs one-minute sounding since 2007. This dataset allows a unique opportunity for investigating possible effects of ultra-low frequency (ULF, 1–7?mHz) waves in the auroral ionosphere. Suitable observations were made during moderately disturbed geomagnetic conditions typically at recovery of the geomagnetic storms caused by solar wind high-speed streams, in the daytime between 9 and 16 MLT. The ionospheric oscillations corresponding to Pc5 geomagnetic pulsations were found in variations of the virtual height of the F layer and the power of ionosonde reflections from E and F layers. The later are most probably caused by modulation of electron precipitation, which is also manifested in weak (about 0.01–0.06?dB) variations of cosmic noise absorption. The most important and novel result is that the pulsations of power of reflection from E and F layers typically has a spectral maximum at nearly half the periodicity of the Pc5 geomagnetic pulsations, whereas such spectral peak is negligible in the geomagnetic pulsations.     

Generation of kinetic Alfvén waves by velocity shear instability on auroral field lines

Ion beams observed in the plasma sheet boundary layer (PSBL), cusp, and on the auroral zone field lines are expected to have spatial gradients in their drift velocity. Generation of kinetic Alfvén waves by velocity shear of the ion beams is discussed. It is shown that a hot ion beam can excite both a resonant kinetic Alfvén wave instability and a non-resonant coupled Alfvén-ion acoustic instability. For typical parameters, observed on the auroral field lines in the altitude range of 5–7 R_E (where R_E is the Earth’s radius), the frequency of the velocity shear modes, in the satellite frame of reference, lie in the ultra-low frequency (ULF) range. The noise due to velocity shear driven Alfvén modes is electromagnetic in nature, and has a finite parallel electric field component.     

Whistler waves in plasmas with time-varying magnetic field: Laboratory investigation

Modulation of whistler waves in a plasma with time-dependant magnetic field perturbations was investigated experimentally. The experiments were performed on large “Krot” device, which was specially designed to study space plasma physics phenomena. It is shown that magnetic field variations on the wave propagation path can lead to splitting of initially continuous whistler wave into the sequence of bursts, whose repetition rate corresponds to magnetic field perturbation period. The frequency inside each burst is changing from its front edge to the back edge. Relative shift of the wave frequency can be as large as the relative magnetic disturbance. Distortion of whistler wave frequency spectrum after its passing through magnetically disturbed areas can be used as a diagnostics for low-frequency magnetic field variations. The applicability of our laboratory results to space plasma is discussed.     

1980年中层大气温度波空间特征的初步分析

利用1980年Nimbus-7卫星网络点资料(温度场)对中层大气行星波的空间结构进行诊断和分析后发现,行星波扰动主要集中于冬半球,夏半球及赤道地区上空的扰动则相对较弱,但也不可忽视.冬半球行星波扰动中的瞬变波部分可以跨过赤道向夏半球传播,且传播主要集中于20kin和70km两个高度层附近.波数1冬季以准定常行里波为主,夏季瞬变行星波与准定常行星波波幅相当.行星波扰动的波幅从冬到夏的衰减主要表现在波数1和波数2上,波数3变化不大.      

空间碎片的空间密度算法研究

由于空间碎片的影响, 空间环境日益恶劣,有必要建立空间碎片环境工程模型对空间碎片撞击航天器进行风险评估.本文研究了空间碎片环境模型中的重要环节, 即碎片的空间密度问题,在统计理论与椭圆轨道理论基础上,分析及推导了空间碎片在空间中的分布状况及空间密度,并得出了碎片空间密度的空间坐标函数解析表达式.同时对引入假设条件的合理性进行了讨论,并利用双行元数据对结论进行了验证, 利用本文方法得出的结果与双行元数据吻合.