半球谐振陀螺控制电路频率跟踪精度提升方法

半球谐振陀螺控制电路的控制精度直接影响半球谐振陀螺仪的输出精度,而频率跟踪精度又直接影响了半球谐振陀螺控制电路的精度.传统的半球谐振陀螺数字控制电路采用过零比较的方法计算陀螺幅点信号的频率,此方法易受地线毛刺信号的干扰,频率跟踪精度不高.介绍了采用A/D转换采集数据估算陀螺幅点信号频率的方法,并对各种方法进行了优缺点比较,提出选用建议.这些方法既提升电路抗干扰能力,又大幅提升了频率跟踪精度,还省去了过零比较电路.分析及测试结果表明,采用该频率跟踪方法,半球谐振陀螺的频率跟踪精度可达0.002Hz,可大幅提升半球谐振陀螺控制电路的精度.     

基于SPCE061A数字四探针电阻率测试仪的设计

以16位单片机SPCE0 6 1A为控制核心,并采用内带程控放大器和片上数字滤波器的16位Σ-Δ型模数转换器AD770 5 ,设计了一款智能四探针电阻率测试仪的硬件电路。该仪器能够自动选择量程和自动校准,本设计减小了印刷电路板的面积,提高了测试仪器的智能化水平,具有一定的实用开发价值。     

热处理工艺对复合熔体处理A356合金组织和性能的影响

利用熔体超声处理、Sr/Ce复合变质及热处理相结合的方法提高铝合金的强韧性,通过金相组织分析及力学性能测试研究了固溶处理对A356合金组织和性能的影响。研究结果表明,熔体处理有利于改善α-Al枝晶和共晶硅相,铸态合金的抗拉强度和伸长率分别达到215 MPa和9.5%;T6热处理后,共晶硅的形态由纤维状转变成独立分布的颗粒状,而除了伸长率之外,合金的力学性能都显著提高;随着固溶时间的延长,共晶硅的等效直径呈现先减小后增大的趋势,而长径比逐渐减小,合金的拉伸性能和硬度均呈现先增大后减小的趋势;当固溶时间为4 h时,合金的综合力学性能达到最佳,其抗拉强度、屈服强度、伸长率和显微硬度分别达到300、240 MPa、8.0%和110HV。     

某弹载计算机GJB1188A接口的设计与实现

栽机要求悬挂物必须实现GJB1188A中数据总线(GJB289A)的远程终端(RT)功能,同时实现GJB1188A中任务悬挂物投放允许等接口功能.描述了一种采用TMS320C6713B高速浮点DSP为核心的GJB1188A接口的实现方法,从硬件平台组成、控制逻辑实现、驱动软件结构三个方面来说明GJB289A(RT)功能的实现方法.介绍了任务悬挂物投放允许等接口的一种设计实现方法.从而将以往单一的GJB289A总线接口模块与嵌入式计算机结合在一起.满足了体积和成本上的要求.使嵌入式弹载计算机在GJB1188A接口的前提下实现与机载火控系统的通信、进行同步的数据采集与控制.     

通过超实时仿真验证轨控策略方法研究

"嫦娥一号"卫星任务中轨道复杂、轨控次数多,为保证每一次轨控的成功,需要考虑各种约束条件制定最优轨控策略,并能得以验证。本文提出通过超实时仿真验证轨控策略的方法,并以某次轨控为例,详细介绍了该方法的实施步骤。通过超实时仿真验证轨控策略可以评估轨控策略的准确性,并实现在任务执行过程中对轨控相关指令的检验。     

嫦娥一号月球探测卫星技术特点分析

嫦娥一号卫星是我国的第一个月球探测卫星,将飞行至距地球380000km的月球,实现环绕月球对其遥感探测。由于任务目标不同,嫦娥一号卫星将遇到比近地轨道卫星更复杂的空间环境和飞行控制过程,所以必须解决面临的所有新技术问题。文章介绍了嫦娥一号卫星在轨道设计、月食、热设计、制导导航、测控、数传等方面的技术特点及研制验证方法。     

KM6气闸舱舱内环境控制技术

文章根据人-船-服试验对KM6气闸舱的要求,分析了舱内环境的几种积累效应,对气闸舱环境控制系统进行了设计,成功地解决了舱内环境控制中CO2置换、低压缺氧以及降压速率等问题,同时配备了气体成分实时监测设备,可以对舱内环境进行严格监测。     

Comparison of Landsat OLI,ASTER, and Sentinel 2A data in lithological mapping : A Case study of Rich area (Central High Atlas,Morocco)

The eastern part of the Rich area consists of the massive Paleozoic and Meso-Cenozoic cover formations that present the geodynamic development of the study area, where is characterized by various carbonate facies of Jurassic age. The geographical characteristic of the study area leaves the zone difficult to map by conventional methods. The objective of this work focuses on the mapping of the constituent lithological units of the study area using multispectral data of Landsat OLI, ASTER, and Sentinel 2A MSI. The processing of these data is based on a precise methodology that distinguishs and highlights the limits of the different lithological units that have an approximate similarity of spectral signature. Three techniques were used to enhance the image including Principal Component Analysis (PCA), Minimum Noise Fraction (MNF), and Independent Component Analysis (ICA). Lithological mapping was performed using two types of supervised classification : Maximum likelihood classifier (MLC) and Support Vector Machine (SVM).The results of processing data show the effectiveness of Sentinel 2A data in mapping of lithological units than the ASTER and Landsat OLI data. The classification evaluation of two methods of the Sentinel 2A MSI image showed that the SVM method give a better classification with an overall accuracy of 93,93% and a Kappa coefficient of 0.93, while the MLC method present an overall accuracy of 82,86% and a Kappa coefficient of 0.80. The results of mapping obtained show a good correlation with the geological map of the study area as well as the efficiency of remote sensing in identification of different lithological units in the Central High Atlas.     

Science objectives of the magnetic field experiment onboard Aditya-L1 spacecraft

The Aditya-L1 is first Indian solar mission scheduled to be placed in a halo orbit around the first Lagrangian point (L1) of Sun-Earth system in the year 2018–19. The approved scientific payloads onboard Aditya-L1 spacecraft includes a Fluxgate Digital Magnetometer (FGM) to measure the local magnetic field which is necessary to supplement the outcome of other scientific experiments onboard. The in-situ vector magnetic field data at L1 is essential for better understanding of the data provided by the particle and plasma analysis experiments, onboard Aditya-L1 mission. Also, the dynamics of Coronal Mass Ejections (CMEs) can be better understood with the help of in-situ magnetic field data at the L1 point region. This data will also serve as crucial input for the short lead-time space weather forecasting models.The proposed FGM is a dual range magnetic sensor on a 6?m long boom mounted on the Sun viewing panel deck and configured to deploy along the negative roll direction of the spacecraft. Two sets of sensors (tri-axial each) are proposed to be mounted, one at the tip of boom (6?m from the spacecraft) and other, midway (3?m from the spacecraft). The main science objective of this experiment is to measure the magnitude and nature of the interplanetary magnetic field (IMF) locally and to study the disturbed magnetic conditions and extreme solar events by detecting the CME from Sun as a transient event. The proposed secondary science objectives are to study the impact of interplanetary structures and shock solar wind interaction on geo-space environment and to detect low frequency plasma waves emanating from the solar corona at L1 point. This will provide a better understanding on how the Sun affects interplanetary space.In this paper, we shall give the main scientific objectives of the magnetic field experiment and brief technical details of the FGM onboard Aditya-1 spacecraft.     

Evaluation of the improvement of IRI-2016 over IRI-2012 at the India low-latitude region during the ascending phase of cycle 24

This paper investigated the performance of the latest International Reference Ionosphere model (IRI-2016) over that of IRI-2012 in predicting total electron content (TEC) at three different stations in the Indian region. The data used were Global Positioning System (GPS) data collected during the ascending phase of solar cycle 24 over three low-latitude stations in India namely; Bangalore (13.02°N Geographic latitude, 77.57°E Geographic longitude), Hyderabad (17.25°N Geographic latitude, 78.30°E Geographic longitude) and Surat (21.16°N Geographic latitude, 72.78°E Geographic longitude). Monthly, the seasonal and annual variability of GPS-TEC have been compared with those derived from International Reference Ionosphere IRI-2016 and IRI-2012 with two different options of topside electron density: NeQuick and IRI01-corr. It is observed that both versions of IRI (i.e., IRI-2012 and IRI-2016) predict the GPS-TEC with some deviations, the latest version of IRI (IRI-2016) predicted the TEC similar to those predicted by IRI-2012 for all the seasons at all stations except for morning hours (0500 LT to 1000?LT). This shows that the effect of the updated version is seen only during morning hours and also that there is no change in TEC values by IRI-2016 from those predicted by IRI-2012 for the rest of the time of the day in the Indian low latitude region. The semiannual variations in the daytime maximum values of TEC are clearly observed from both GPS and model-derived TEC values with two peaks around March-April and September-October months of each year. Further, the Correlation of TEC derived by IRI-2016 and IRI-2012 with EUV and F10.7 shows similar results. This shows that the solar input to the IRI-2016 is similar to IRI 2012. There is no significant difference observed in TEC, bottom-side thickness (B0) and shape (B1) parameter predictions by both the versions of the IRI model. However, a clear improvement is visible in hmF2 and NmF2 predictions by IRI-2016 to that by IRI-2012. The SHU-2015 option of the IRI-2016 gives a better prediction of NmF2 for all the months at low latitude station Ahmedabad compare to AMTB 2013.