磁通门磁强计校准装置研究

本文介绍了磁通门磁强计校准装置的系统组成，包括大开口大均匀区的三轴磁场线圈、磁场线圈非均匀性的补偿方法、三轴磁场线圈非正交性补偿方法、串并联组合磁场线圈分流电路等，分析了校准装置的测量不确定度主要来源，给出了验证结果。该装置可开展磁通门磁强计（含传感器）示值误差、线性度、正交度等参数的校准，其成果已应用于十多家单位的磁场测试系统和数十家单位的磁通门磁强计校准。     

磁通门磁强计校准装置研究

本文介绍了磁通门磁强计校准装置的系统组成,包括大开口大均匀区的三轴磁场线圈、磁场线圈非均匀性的补偿方法、三轴磁场线圈非正交性补偿方法、串并联组合磁场线圈分流电路等,分析了校准装置的测量不确定度主要来源,给出了验证结果。该装置可开展磁通门磁强计(含传感器)示值误差、线性度、正交度等参数的校准,其成果已应用于十多家单位的磁场测试系统和数十家单位的磁通门磁强计校准。     

舰船现场计量校准环境模拟装置研究

针对原有舰船装备技术状态的压力和电工类仪器仪表计量时，因所处环境较恶劣，存在温湿度、电磁环境、振动等参数不能满足要求而无法开展计量校准工作的问题，设计了一种基于舰船现场计量校准环境的模拟装置。该装置由环境控制和校准操作两部分组成，重点研究了高温环境下的恒温、恒湿技术，以及分体式校准舱结构设计，实现了微环境的自动调节与控制，通过性能试验，证明了校准舱的温度波动度和均匀度均符合设计指标，能够解决现场计量校准的环境条件保障问题。     

制动式正弦法动态扭矩传感器校准装置设计

针对目前静态扭矩校准无法完全满足使用需求的问题,设计了一种制动式正弦法动态扭矩传感器校准装置,利用伺服电机、磁粉制动器等装置组成制动扭矩激励系统,用标准惯量盘作为负载,用圆光栅测量惯量盘扭摆的角加速度,将动态扭矩溯源至惯量和角加速度参数。通过建模和数值分析,阐述了校准装置的工作原理,利用研制的校准装置样机进行激励试验,试验结果证明了设计思路的可行性。     

100kHz~1MHz频率范围水听器灵敏度激光法校准及其验证

激光法校准水听器灵敏度是一种绝对校准方法，本文介绍了激光法水声声压校准装置的校准原理及主要系统构成，采用激光法对TC4034和BK8103水听器的灵敏度在100kHz~1MHz频率范围进行了校准实验研究，分析了激光法校准装置的测量不确定度，校准结果与三换能器互易法对校准结果进行了对比。结果表明两种校准方法的结果总体上是一致的，校准结果偏差小于两套装置的合成不确定度。本文对导致二者之间偏差的原因进行了分析。     

振动传感器的低频校准

本文介绍了为校准低频振动传感器而研制的低频振动标准装置。从装置的工作原理、组成、技术指标和校准方法到装置所采用的先进技术以及系统的测试和精度分析等方面都作了较详细的论述,从理论到实践初步解决了振动传感器的低频校准问题。     

集成运算放大器参数测试仪校准技术研究

集成运算放大器参数测试仪在国家电子行业中广泛使用,其参数测试质量无法保证。研究了集成运放参数测试仪器采用的“闭环测试原理”和目前存在的三种集成运放参数测试仪的校准方案,建立了集成运放参数测试仪校准装置,实现了集成运放参数测试仪的自动化校准。     

振动与冲击传感器的温度响应校准

振动与冲击传感器的灵敏度(校准系数)、阻尼比和谐振频率均为温度的函数。灵敏度随温度变化的特性称之为温度响应。从分析目前传感器温度响应测试方法存在的问题入手,着重介绍了将激光测振应用于温响校准的实施方法、原理和校准装置的技术性能。     

低频微弱磁场测量仪校准装置研究

本文介绍了低频微弱磁场测量仪校准装置的系统组成、工作原理及各主要组成部分,分析了校准装置的不确定度主要来源,给出了试验验证结果,并提出了后续研究的方向。     

正压漏孔校准装置的设计

正压漏孔校准装置是一种校准气体漏率的计量标准设备 ,可采用定容法和定量气体动态比较法对正压漏孔校准 ,校准范围为 10 2～ 5× 10 - 5 Pa· L /s。该文介绍正压漏孔校准装置的校准原理 ,设计方法 ,参数选取。     

微型镓场发射电推力器的研制和点火特性

为了满足立方星等微纳航天器对推进系统的需求,研制出中国首台针式微型镓场发射电推力器。通过提高润湿温度解决了真空环境下镓难以充分润湿钨针等问题。实现了推力器的稳定点火,测试了不同润湿温度和不同几何参数下的点火特性。得到了发射电流随润湿温度提高、极间距减小和吸极内孔直径的增大而增大的关系。通过公式计算,给出了不同发射电流下的理论推力。通过电场仿真得到不同几何参数下的电场强度,揭示了几何参数影响发射电流的原因。     

脉冲多普勒雷达导引头目标回波模拟器校准技术研究

本文提出采用软件无线电技术实现某型脉冲多普勒雷达导引头目标回波模拟器的校准。使用频谱仪及示波器组成校准装置实现被校信号射频到中频的变换及A/D转换,使用LabVIEW软件实现A/D转换后信号的数字正交解调及参数提取算法,进而实现雷达导引头目标模拟器的脉冲幅度、多普勒频率及延时参数的自动校准。     

空间相机热平衡试验温度预测方法改进及应用

为实现对航天器热平衡试验平衡温度的预测,建立了热平衡温度预测的方程式,对影响预测结果的各参数进行了分析。首先,由节点网络法推导出平衡温度表达式,介绍了其基于非线性最小二乘法的求解过程,建立了平衡温度的迭代方程;其次,结合大量的试验数据,对影响迭代结果的3个因素进行了统计分析,并最终确定了各因素的合理取值范围;最后,利用温度预测程序对某空间相机热平衡试验中低温工况的平衡温度进行了预测,并与试验结束后的结果进行了对比。结果表明,预测温度与试验数据的误差为±1℃（在3%之内）,满足精度要求,对热平衡温度准确的预测有效的缩短了试验时间,节省试验费用。     

The resonance cone technique for exciting electron acoustic waves in equatorial ionosphere

A rocketborne R.F. resonance cone technique is discussed in this paper. The technique is ideal over the geomagnetic equator where the earth's magnetic field is horizontal. The R.F. exciter is fixed along the axis of the rocket. By measuring the semi-angle of this cone various plasma parameters can be derived, such as electron density and temperature.     

Development and performance evaluation of tropospheric scintillation model on Ku-band satellite link over Akure,Nigeria

Existing amplitude scintillation prediction models often perform less satisfactorily when deployed outside the regions where they were formulated. This necessitates the need to evaluate the performance of scintillation models developed in one region using data data from other regions while documenting their relative errors. Due to its variation with elevation angle, frequency, other link parameters and meteorological factors, we employed three years (January 2016 to December 2018) of concurrently measured satellite radio beacons and tropospheric weather parameters to develop a location-based amplitude scintillation prediction model over the Earth-space path of Akure (7.17^oN, 5.18^oE), South-western Nigeria. The satellite beacon measurement used Tektronix Y400 NetTek Analyzer at 1 s integration time while meteorological parameters, namely; temperature, pressure and relative humidity were measured using Davis Vantage Vue weather station at 1 min integration time. Comparative study of the model’s performance with nine (9) existing scintillation prediction models indicates that the best and worst performing models, in terms of root mean square error (RMSE), are the Statistical Temperature and Refractivity (STN) and direct physical and statistical prediction (DPSP) models with values 11.48 and 51.03 respectively. Also, worst month analysis indicates that April, with respective enhancement and fade values of 0.88 and 0.90 dB for 0.01% exceedance, is the overall worst calendar month for amplitude scintillation.     

电推进羽流诊断中阻滞势分析器的快速处理算法

介绍了一种基于统计方法分析阻滞势分析器响应曲线的数据处理算法. 该算法可以在电推进诊断中快速提取待测粒子的环境参数. 通过对阻滞势分析器测量得到的U-I响应曲线物理性质的分析, 推导出以曲线中所有测量值为基础提取粒子温度和密度的统计处理算法. 以具体卫星电推进诊断中对阻滞势分析器的测量要求以及工程参数为例, 设计并进行了仿真模拟实验. 在设计要求的测量范围内, 利用本文算法得到的离子密度的平均误差为6.62 %, 粒子温度的平均误差为7.45 %. 通过分析算法运算量, 在实际工程中采用12 MHz主频的8031处理器可以在0.5 s内完成本算法全部处理过程.      

Effects of electrostatic forces on the vertical structure of planetary rings

We have calculated the vertical structure of planetary dust rings as it results from a balance between an electrostatic force on the dust grains and the vertical component of the gravitational force from the central planet. The electrostatic force results from the charging of the dust grains by the ambient plasma and a large scale electric field due to a shielding electric field and the resulting vertical dust distribution are strongly dependent on dust size, dust and plasma density, plasma temperature and plasma ion type. The dust density distribution has a different dependence on these parameters in tenuous and in dense dust rings. We solve the relevant equations numerically and also by linearization in the limiting cases of tenuous or dense rings. Our results indicate that the effects treated in this paper may be important in both Jupiter's and Saturn's rings.     

交流量子化霍尔效应的研究与应用

电阻有频率变差,电阻在交流状态下的溯源是计量领域的难题,以往采用交直流差可计算电阻实现了交流电阻的溯源,但存在稳定性和一致性较差的问题,当前采用交流量子化霍尔效应作为交流电阻标准成为计量领域的研究热点。其中需要解决交流量子化霍尔电阻及其向实物标准电阻传递的准确度问题。本文介绍了采用分裂式屏蔽结构克服交流量子化霍尔电阻频率误差的方法,研制10-8量级高准确度四端对电桥满足交流量子电阻的传递需求,研制完全等电位屏蔽结构的交流电桥校准装置保证四端对电桥的准确度,并介绍了交流量子电阻基准的应用领域。     

Solar sailing in realistic mode,based on a locally-optimal control laws

Ballistic design of solar sailing missions in the solar system is composed of defining the design parameters, the control programs, and the trajectories that provide performance goals of a flight. The use of a solar sail spacecraft imposes specific restrictions on mission parameters that include the degradation limit on the flight duration, the maximum temperature of solar sail's surface, the minimum distance from the Sun, the maximum angular velocity of the spacecraft's rotation and others.Many authors considered the impact of these restrictions on the design of the mission separately, but they used a sophisticated method of finding the exact optimal motion control or applied the most straightforward laws of motion control. This paper uses local-optimal control laws at the complete mathematical models of motion and functioning of solar sail spacecraft to describe a technique of designing interplanetary missions. The described method avoids the need to obtain an accurate optimal solution to the control problem and does not cause significant computational difficulties.     

Study of VLF wave with relativistic effect in Saturn magnetosphere in the presence of parallel A.C. electric field

Cassini radio and plasma wave surveys aim to study radio emissions, plasma waves, thermal plasma and dust near Saturn. Using the characteristic solution and dynamics method, the influence of electron beam on the loss cone and bi-Maxwellian distribution of whistler mode waves in the parallel alternating electric field and magnetic field is studied. The dispersion relation and the growth rate of Saturn's magnetic layer were deduced and calculated in detail. Parameter analysis is performed by changing the parameters of the plasma like number density, AC frequency, temperature anisotropy, etc. The influence of AC frequency on Doppler shift and the comparative study of growth rate of oblique and parallel propagating waves are analyzed using generalized distribution function. We found temperature anisotropy ${\text{A}}_{\text{T}}=1.25$ can explain the linear spatiotemporal growth rate of whistler mode waves. It provides the majority of the observed frequency integral power. It can be seen that the effective parameters for the generation of Whistler mode waves are not only temperature anisotropy, but also the relativistic factors discussed in the results and discussion section, and the AC field frequency and width of the loss cone distribution function.