空间目标双基地ISAR一维距离像速度补偿方法

空间目标的高速运动会造成双基地ISAR一维距离像的畸变,针对此问题,研究了相应的速度估计与补偿方法。基于中频直接采样匹配滤波非相参双基地ISAR成像系统,首先研究了高速运动对双基地ISAR成像的影响,其次利用雷达基带回波具有的稀疏性,构造出与高速运动目标回波特性相匹配的冗余基并对其进行稀疏分解,然后据此估计出回波的调频斜率,进而估计出目标的无模糊速度,最后构造补偿相位项完成对宽带回波的速度补偿。算法补偿精度高,且无测速模糊,空间目标理想散点的仿真实验验证了补偿方法的有效性。     

基于虚拟仪器的无线电设备检测仪

ATE是军用飞机测试技术的发展方向,利用虚拟仪器开发机载无线电台的检测系统是向ATE发展的重要一步。目前成熟的总线技术和虚拟仪器技术提供了技术实现途径,为此基于虚拟仪器技术设计了无线电设备的地面检测仪。     

航天测量船外测数据误差分析的小波方法

使用动态数据建模与误差分离技术以及小波分频方法,对船载外测数据进行处理分析,成功地分离出随机误差和船测数据特有的船体误差,并对船体误差给出了分析和合理的解释。结论表明,小波分频对认识和研究船测数据的误差是一种非常有效的方法。     

Probing the first stars and black holes in the early Universe with the Dark Ages Radio Explorer (DARE)

A concept for a new space-based cosmology mission called the Dark Ages Radio Explorer (DARE) is presented in this paper. DARE’s science objectives include: (1) When did the first stars form? (2) When did the first accreting black holes form? (3) When did Reionization begin? (4) What surprises does the end of the Dark Ages hold (e.g., Dark Matter decay)? DARE will use the highly-redshifted hyperfine 21-cm transition from neutral hydrogen to track the formation of the first luminous objects by their impact on the intergalactic medium during the end of the Dark Ages and during Cosmic Dawn (redshifts z = 11–35). It will measure the sky-averaged spin temperature of neutral hydrogen at the unexplored epoch 80–420 million years after the Big Bang, providing the first evidence of the earliest stars and galaxies to illuminate the cosmos and testing our models of galaxy formation. DARE’s approach is to measure the expected spectral features in the sky-averaged, redshifted 21-cm signal over a radio bandpass of 40–120 MHz. DARE orbits the Moon for a mission lifetime of 3 years and takes data above the lunar farside, the only location in the inner solar system proven to be free of human-generated radio frequency interference and any significant ionosphere. The science instrument is composed of a low frequency radiometer, including electrically-short, tapered, bi-conical dipole antennas, a receiver, and a digital spectrometer. The smooth frequency response of the antennas and the differential spectral calibration approach using a Markov Chain Monte Carlo technique will be applied to detect the weak cosmic 21-cm signal in the presence of the intense solar system and Galactic foreground emissions.     

The Scanning Sky Monitor (SSM) on ASTROSAT

The Scanning Sky Monitor is one of the experiments onboard the ASTROSAT, an Indian multiwavelength astronomy satellite mission. This experiment will detect and monitor X-ray transients in the energy band 2–10 keV. It is similar in design to the ASM on RXTE. It consists of position-sensitive proportional counters with one-dimensional mask. We describe the configuration of the experiment. We also discuss some of the results obtained using a detector which has already been fabricated and tested in our laboratory.     

一种新型综合性靶场安全系统及其检验测试结果

本文首先简要介绍战略导弹发射场和航天发射场靶场安全系统的作用、特点、主要技术要求,接着介绍按美国空军航天司令部要求,由空军研究所开发的基于GPS弹道测量技术,外测、遥测、遥控综合为一体的机动型靶场安全系统——BMRST的构成及其经多种检验测试的结果。     

三点测距副站技术

设计和研制的两个副站（乌鲁木齐站和广州站）和北京的主站相互配合形成三点测距系统,可以完成对风云二号卫星的测距定轨任务。文章着重介绍了副站的组成、作用和功能技术指标等。它的设计方法与国外同类技术相比颇具特色。经过对日本气象卫星进行的几年跟踪测试,及最后通过对风云二号卫星执行任务的验证,确认了副站方案的可行性,设计的合理性。     

一种适用于大场景圆迹环扫SAR的改进CS成像算法

在宽测绘带圆迹环扫合成孔径雷达(CSSAR)中,目标斜距表示形式复杂,测绘带内距离徙动(RCM)变化剧烈均给成像处理引入难点。针对上述问题,根据圆迹环扫SAR平台的运动特性,使用高阶逼近的方法建立圆弧曲线模型下的回波信号斜距方程,并以导出的二维频谱高阶近似解析表达式为基础,考虑大场景下的距离徙动空变问题,对空变的斜距历程进行详细的分析,并提出了一种适用于大场景圆迹环扫SAR的改进线性调频变标(CS)成像算法。仿真结果说明,曲线模型的斜距方程精度较高,该算法能够精确校正空变的距离徙动,对较大场景取得了较好的成像效果。     

Improved interpretation of solar wind ion measurements via high-resolution magnetic field data

The Wind   spacecraft’s Faraday cups (FC) continue to produce high-quality, in situ observations of thermal protons (i.e., ionized hydrogen) and α$\alpha$-particles (i.e., fully ionized helium) in the solar wind. By fitting a Wind/FC ion spectrum with a model velocity distribution function (VDF) for each particle species, values for density, bulk velocity, and temperature can be inferred. Incorporating measurements of the background magnetic field from the Wind Magnetic Field Investigation (MFI) allows perpendicular and parallel temperature components to be separated. Prior implementations of this analysis averaged the higher-cadence Wind/MFI measurements to match that of the Wind/FC ion spectra. However, this article summarizes recent and extensive revisions to the analysis software that, among other things, eliminate such averaging and thereby account for variations in the direction of the magnetic field over the time taken to measure the ions. A statistical comparison reveals that the old version consistently underestimates the temperature anisotropy of ion VDF’s: averaging over fluctuations in the magnetic field essentially blurs the perpendicular and parallel temperature components, which makes the plasma seem artificially more isotropic. The new version not only provides a more accurate dataset of ion parameters (which is well suited to the study of microkinetic phenomena), it also demonstrates a novel technique for jointly processing particle and field data. Such methods are crucial to heliophysics as wave-particle interactions are increasingly seen as playing an important role in the dynamics of the solar wind and similar space plasmas.     

Mercury Ion Analyzer (MIA) onboard Mercury Magnetospheric Orbiter: MMO

The Mercury Magnetopsheric Orbiter (MMO) is one of the spacecraft of the BepiColombo mission; the mission is scheduled for launch in 2014 and plans to revisit Mercury with modern instrumentation. MMO is to elucidate the detailed plasma structure and dynamics around Mercury, one of the least-explored planets in our solar system. The Mercury Plasma Particle Experiment (MPPE) on board MMO is a comprehensive instrument package for plasma, high-energy particle, and energetic neutral particle atom measurements. The Mercury Ion Analyzer (MIA) is one of the plasma instruments of MPPE, and measures the three dimensional velocity distribution of low-energy ions (from 5 eV to 30 keV) by using a top-hat electrostatic analyzer for half a spin period (2 s). By combining both the mechanical and electrical sensitivity controls, MIA has a wide dynamic range of count rates for the proton flux expected around Mercury, which ranges from 10⁶ to 10¹² cm⁻² s⁻¹ str⁻¹ keV⁻¹, in the solar wind between 0.3 and 0.47 AU from the sun, and in both the hot and cold plasma sheet of Mercury’s magnetosphere. The geometrical factor of MIA is variable, ranging from 1.0 × 10⁻⁷ cm² str keV/keV for large fluxes of solar wind ions to 4.7 × 10⁻⁴ cm² str keV/keV for small fluxes of magnetospheric ions. The entrance grid used for the mechanical sensitivity control of incident ions also work to significantly reduce the contamination of solar UV radiation, whose intensity is about 10 times larger than that around Earth’s orbit.