低噪声500MHz频率源

本文介绍一种高可靠、长寿命频率源的设计。为了可靠的工作,该装置采用了备用结构型式,并用体波和声表面波谐振器来保证极低的相位噪声和寄生输出。500MHz 和400MHz 多路输出是由25MHz 参考输入或由一个内部100MHz 温度补偿晶体振荡器直接合成而产生的。当使用外部参考时,25MHz 输入滤波器和两个50MHz、100MHz 附加晶体滤波器保证在最后倍频之前将相位噪声本底减小到理论最小值。500MHz 倍频输出信号用两端口SAW 谐振器进行滤波。这些谐振器在50欧匹配系统中,工作的输入功率电平为+15dBm。滤波电路还保证将内外产生的调制边带减小到可以忽略的程度。在离载波大于2MHz 间隔频率上,其单边带相位噪声低于-174dBc/Hz。同样,在所有频率上,寄生信号均低于-110dBc。频率源工作在有电噪声的环境中。良好的有源、无源滤波和封装屏蔽可保证最小的导电和辐射敏感性。对系统的苛刻要求决定采用无单点故障的备用重复结构。提出的封装设想是使组件的内部连接最短,并使两个备用发生器在物理和电气上互不相关。     

一种静电计运算放大器测试电路设计

为提高直流微电流测量的准确度,对测量原理电路的噪声进行分析,确定不同噪声对直流微电流测量的影响,选定低噪声测量原则。对测量结果误差进行分析,得到电路中反馈电阻最大允许误差、运算放大器的输入偏置电流、失调电压为主要影响因素,并根据实际元器件进行举例分析验证。静电计运算放大器对测量误差的影响仍不可忽略,设计电路测量其关键指标,针对微弱电流信号的特点采取屏蔽、保护措施,搭建测试电路,测试筛选出低输入偏置电流、低失调电压的静电计运算放大器应用在高精度源表中。     

FPGA在超周期延时电路中的应用

一般电路的暂态输出时间相对不是很长 ,而且电路的输入触发信号时间应小于输出时间的长度 ,这种电路设计思想有时满足不了某些场合的实际工程需要。为此 ,本文结合工程实际需要给出了利用FPGA设计超周期延时功能模块 ,该模块能准确的进行时序控制 ,可以不修改硬件满足时序要求。     

基于相关双采样技术的CCD视频信号处理研究

在动态目标的CCD探测中,一个非常关键的技术就是对CCD输出信号噪声的抑制或削弱,以提高输出信号的信噪比。首先,对CCD输出信号的特性及常用处理方法进行了简要描述,并结合CCD输出噪声的特点,对相关双采样(Correlated Double Sampling)法进行了细致地分析。最后在建立CDS传输函数及噪声分析模型的基础上,利用最适合的相关双采样技术对CCD信号存在的复位噪声及其它低频噪声的抑制进行了相关测试。结果表明:对2δ法CDS电路,只要选择合适的采样时间,不仅能有效地消除KTC噪声,而且对低频噪声及其它白噪声也有不同程度的抑制。     

MEMS陀螺噪声理论与模型综述

工作在闭环检测模式下的MEMS陀螺具有较好的整体性能,是目前具有发展潜力的微陀螺方案之一。但是多个闭环的存在使得测控系统噪声源变多,通过构建噪声模型可以量化各噪声源对零偏输出的贡献,并且探明结构和电路参数对噪声性能指标的影响,从而调整设计参数与控制方式,优化设计。首先阐述了MEMS陀螺谐振系统中的噪声源———热噪声和闪频噪声产生机理,然后将陀螺噪声模型分为相位噪声模型和幅度噪声模型,分别讨论国内外研究机构噪声建模的进展,如针对幅度频率耦合导致的额外相位噪声,讨论了非线性相位噪声模型和幅度噪声模型。非线性相位噪声模型通过引入非线性刚度来完善相位噪声谱表达式,幅度噪声模型通过考虑不同输入点的噪声在力平衡环路的传递过程来量化各噪声源影响因素。最后,对噪声模型的发展进行了展望,可以通过构建与调幅陀螺相联系的相位噪声模型和零偏不稳定性噪声模型,实现对陀螺噪声分析的完善。     

利用同步检测的频率比较器

监测频率有许多种不同的方法,但其中绝大多数均有这样的缺点,即在监测时,总会把与所需波形同时存在于电路内的固有噪声测出。本文的电路克服了这个噪声问题。它采用的方法是以参考信号的频率对未知频率的信号采样,然后用一个低通滤波器得出被测波形的平均詹。如果输入频率 f_(in)等于参考频率 f_(ref),则在输出端产生一个不等于零的平均值。而如果是 f_(in)≠f_(ref),则各采样值的平均值等于零。除此之外,该电路对噪声是无响应的。它能在100赫至100千赫范围内很好地工作。     

一种基于APFC的大功率LED驱动电路的研究

研究了一种基于Boost原理的大功率LED驱动电路,采用有源功率因数校正（APFC）技术,选择平均电流控制法控制电路,一个电流环和一个电压环组成双闭环控制系统,使输入电流跟踪输入电压,以实现功率因数校正及降低输入端总谐波畸变的目的。基于PSIM软件进行仿真研究,得到了理想的效果,验证了该LED驱动电路的可行性。     

基于Push-Push结构的倍频器在铷原子频标中的应用

铷原子频标是各种原子频标中发展最为活跃的 ,由于其独特的外在及内在的特点 ,使其在商业通信、空间导航等领域得到最为广泛的应用。在铷原子频标中 ,倍频电路是影响整个系统长期稳定性的重要因素之一。简要介绍了Push -Push结构的基本原理 ,并且给出了基于Push -Push结构的倍频器的具体实现电路与仿真结果。仿真实验结果表明 ,该种结构设计对改善电路的相位噪声是有十分有效的。最后分析了影响幅度调制噪声与相位调制噪声的因素 ,对上述电路做了进一步的完善。     

射频脉冲序列随机起伏的数据采集

数据采集系统是射频脉冲序列脉间频率稳定度测试系统中的一部分。该系统由微波部分、视频电路及数据采集部分构成。它用于测量雷达脉间相位噪声。射频脉间相位噪声经过微波检测电路、视频电路后变成随机起伏的视频脉冲信号。数据采集就是对脉冲信号采样、模数转换,将一段连续采集的数据存入微机。着重讨论数据采集的工作原理、采集电路的构成、几种采集方法,最后对采集精度及动态进行了分析。     

电位器轨道噪声的机理分析及实验研究

前言电位器旋转噪声的研究是涉及到我国电位器生产工艺与检验技术的一个迫切问题。长期以来,IEC 组织对轨道噪声的测试未做原则性修改,所推荐的测试电路一直沿袭至今。近十多年来,我国在噪声测试仪器的研制方面做了很多工作。对噪声机理的研究与工艺改革则更是大多数生产和研究单位着重进行的工作之一。从测试的角度很希望研制出在可比性和测试速度方面都得到提高的仪器。从工艺研究的角度也希望从测试实验中分析噪声机理找出提高质量的途径。本文是作者对轨道噪声特性的实验研究报     

Space flight, microgravity, stress, and immune responses.

Exposure of animals and humans to space flight conditions has resulted in numerous alterations in immunological parameters. Decreases in lymphocyte blastogenesis, cytokine production, and natural killer cell activity have all been reported after space flight. Alterations in leukocyte subset distribution have also been reported after flight of humans and animals in space. The relative contribution of microgravity conditions and stress to the observed results has not been established. Antiorthostatic, hypokinetic, hypodynamic, suspension of rodents and chronic head-down tilt bed-rest of humans have been used to model effects of microgravity on immune responses. After use of these models, some effects of space flight on immune responses, such as decreases in cytokine function, were observed, but others, such as alterations in leukocyte subset distribution, were not observed. These results suggest that stresses that occur during space flight could combine with microgravity conditions in inducing the changes seen in immune responses after space flight. The biological/biomedical significance of space flight induced changes in immune parameters remains to be established. Grant Numbers: NCC2-859, NAG2-933.     

Turbulence,complexity, and solar flares

The issue of predicting solar flares is one of the most fundamental in physics, addressing issues of plasma physics, high-energy physics, and modelling of complex systems. It also poses societal consequences, with our ever-increasing need for accurate space weather forecasts. Solar flares arise naturally as a competition between an input (flux emergence and rearrangement) in the photosphere and an output (electrical current build up and resistive dissipation) in the corona. Although initially localised, this redistribution affects neighbouring regions and an avalanche occurs resulting in large scale eruptions of plasma, particles, and magnetic field. As flares are powered from the stressed field rooted in the photosphere, a study of the photospheric magnetic complexity can be used to both predict activity and understand the physics of the magnetic field. The magnetic energy spectrum and multifractal spectrum are highlighted as two possible approaches to this.     

论精大贵稀仪器仪表潜在功能的开发

精大贵稀仪器仪表潜在功能的开发,充分利用了现有资源,节省大量的更新经费,产生了巨大的技术、经济效益.在市场经济机制下,开展共用协作,极大地改善了精大贵稀仪器利用率低的状况,且有一定的推广应用前景,为培养、锻炼年轻的技术人员,以点带面地推动人员技术素质的全面提高起了积极的作用.     

Determination of K,Ar, Cl,S, Si and Al flare abundances from RESIK soft X-ray spectra

The RESIK is a high sensitivity, uncollimated bent crystal spectrometer which successfully operated aboard Russian CORONAS-F solar mission between 2001 and 2003. It measured for the first time in a systematic way solar soft X-ray spectra in the four wavelength channels from 3.3 Å to 6.1 Å. This range includes characteristic strong lines of H- and He-like ions of K, Ar, Cl, Si, S and Al in the respective spectral channels. A distinguishing feature of RESIK is its possibility of making reliable measurements of the continuum radiation in flares. Interpretation of line and the continuum intensities observed in vicinity of respective strong lines provides diagnostics of plasma temperature and absolute abundances of K, Ar, Cl, S, Si and Al in several flares. We analyzed the observed intensities of spectral lines and the nearby continuum using the CHIANTI v5.2 atomic data package. A specific, so-called “locally isothermal” approach has been used in this respect allowing us to make not only flare-averaged abundance estimates, but also to look into a possible variability of plasma composition during the course of flares.     

Probable interstellar MgX (X = CN, NC, CCH, CC, C3N, NCCC, CCNC, C4H, and C4): A DFT study

The geometries, dipole moments, and rotational constants for several magnesium compounds and their anions were calculated by using the B3LYP/Aug-cc-pVTZ method. The rotational constants of linear forms have been derived to be used for laboratory experiment and astronomical observation.     

Advancing participation of blind students in Science,Technology, Engineering,and Math

Like their sighted peers, many blind students in elementary, middle, and high school are naturally interested in space. This interest can motivate them to learn fundamental scientific, quantitative, and critical thinking skills, and sometimes even lead to careers in Science, Technology, Engineering, and Math (STEM) disciplines. However, these students are often at a disadvantage in science because of the ubiquity of important graphical information that is generally not available in accessible formats, the unfamiliarity of teachers with non-visual teaching methods, lack of access to blind role models, and the low expectations of their teachers and parents. We discuss joint efforts by the National Aeronautics and Space Administration (NASA) and the National Federation of the Blind’s (NFB) National Center for Blind Youth in Science (NCBYS) to develop and implement strategies to promote opportunities for blind youth in science. These include the development of tactile space science books and curriculum materials, science academies for blind middle school and high school students, and college-level internship and mentoring programs. The partnership with the NFB exemplifies the effectiveness of collaborations between NASA and consumer-directed organizations to improve opportunities for underserved and underrepresented individuals.     

The giant planets and their satellites: Report on the Cospar Symposium,Ottawa, Canada,May 18–21, 1982

A $\text{Symposium on the Giant Planets and Their Satellites}$ was presented in conjunction with the Twenty-fourth Plenary Meeting of the Committee on Space Research. This paper summarizes the talks presented and places the remaining papers of this volume in context.     

Utilization of CAM,CAF, MAX,and FAX for space radiation analyses using HZETRN

To estimate astronaut health risk due to space radiation, one must have the ability to calculate various exposure-related quantities that are averaged over specific organs and tissue types. Such calculations require computational models of the ambient space radiation environment, particle transport, nuclear and atomic physics, and the human body. While significant efforts have been made to verify, validate, and quantify the uncertainties associated with many of these models and tools, relatively little work has focused on the uncertainties associated with the representation and utilization of the human phantoms. In this study, we first examine the anatomical properties of the Computerized Anatomical Man (CAM), Computerized Anatomical Female (CAF), Male Adult voXel (MAX), and Female Adult voXel (FAX) models by comparing the masses of various model tissues used to calculate effective dose to the reference values specified by the International Commission on Radiological Protection (ICRP). The MAX and FAX tissue masses are found to be in good agreement with the reference data, while major discrepancies are found between the CAM and CAF tissue masses and the reference data for almost all of the effective dose tissues. We next examine the distribution of target points used with the deterministic transport code HZETRN (High charge (Z) and Energy TRaNsport) to compute mass averaged exposure quantities. A numerical algorithm is presented and used to generate multiple point distributions of varying fidelity for many of the effective dose tissues identified in CAM, CAF, MAX, and FAX. The point distributions are used to compute mass averaged dose equivalent values under both a galactic cosmic ray (GCR) and solar particle event (SPE) environment impinging isotropically on three spherical aluminum shells with areal densities of 0.4 g/cm², 2.0 g/cm², and 10.0 g/cm². The dose equivalent values are examined to identify a recommended set of target points for each of the tissues and to further assess the differences between CAM, CAF, MAX, and FAX. It is concluded that the previously published CAM and CAF point distributions were significantly under-sampled and that the set of point distributions presented here should be adequate for future studies involving CAM, CAF, MAX, or FAX. It is also found that the errors associated with the mass and location of certain tissues in CAM and CAF have a significant impact on the mass averaged dose equivalent values, and it is concluded that MAX and FAX are more accurate than CAM and CAF for space radiation analyses.     

Debris flux comparisons from the Goldstone Radar,Haystack Radar,and Hax Radar prior,during, and after the last solar maximum

The continual monitoring of the low Earth orbit (LEO) debris environment using highly sensitive radars is essential for an accurate characterization of these dynamic populations. Debris populations are continually evolving since there are new debris sources, previously unrecognized debris sources, and debris loss mechanisms that are dependent on the dynamic space environment. Such radar data are used to supplement, update, and validate existing orbital debris models. NASA has been utilizing radar observations of the debris environment for over a decade from three complementary radars: the NASA JPL Goldstone radar, the MIT Lincoln Laboratory (MIT/LL) Long Range Imaging Radar (known as the Haystack radar), and the MIT/LL Haystack Auxiliary radar (HAX). All of these systems are highly sensitive radars that operate in a fixed staring mode to statistically sample orbital debris in the LEO environment. Each of these radars is ideally suited to measure debris within a specific size region. The Goldstone radar generally observes objects with sizes from 2 mm to 1 cm. The Haystack radar generally measures from 5 mm to several meters. The HAX radar generally measures from 2 cm to several meters. These overlapping size regions allow a continuous measurement of cumulative debris flux versus diameter from 2 mm to several meters for a given altitude window. This is demonstrated for all three radars by comparing the debris flux versus diameter over 200 km altitude windows for 3 nonconsecutive years from 1998 to 2003. These years correspond to periods before, during, and after the peak of the last solar cycle. Comparing the year to year flux from Haystack for each of these altitude regions indicate statistically significant changes in subsets of the debris populations. Potential causes of these changes are discussed. These analysis results include error bars that represent statistical sampling errors.