星载合成孔径雷达模糊特性研究

在分析星载合成孔径雷达模糊信号来源的同时，论述了分辨率，测绘带宽，模糊度，脉冲重复频率之间的相互制约关系，并提出了在总体设计中如何选择脉冲重复频率以减少模糊的方法，最后给出了计算方位模糊比和距离模糊比的实用算法及仿真结果。     

蚁群算法在DGPS动态整周模糊度解算中的应用

在基线长度已知的情况下,利用零空间约束动态求解GPS双差整周模糊度,进行解的去相关后,应用蚁群算法在整周模糊度空间内寻优。根据实测算例解算结果,蚁群算法在很少的解样本数内获得了很好的搜索结果,与遗传算法结果相比较,证明了蚁群算法在相同搜索率的情况下,具有更高的搜索可靠性。     

新型高精度快速单站无源定位技术研究

提出了一种低信噪比条件下基于可变基线数字干涉仪的新型高精度快速单站无源定位算法,给出了系统设计方案。该方案具有诸多优点,有较为广阔的应用前景。     

一种组合型的探干一体化信号设计分析

针对雷达信号资源利用率有待提升、低截获性能不足的问题,提出 1种复合调制的创新型探干一体化信号波形。线性调频信号本身具有良好的低截获性能,伪随机码序列分量具有较好的干扰性,同时又能一定程度上扩展信号带宽,两者的复合调制信号具有良好的探测和干扰性能。对基于 LFM的探干一体化信号波形进行了调制原理分析,并分别从时域、频域、功率谱、模糊函数、自相关特性等角度分析其探测、干扰特性。仿真实验证明,相较于单一调制的线性调频信号,一体化信号具有更宽的频带、更优良的干扰特性和探测性能,同时,有更高效的雷达资源利用率。     

Mitigation of receiver biases in ionospheric observables from PPP with ambiguity resolution

PPP (Precise Point Positioning) is a GNSS (Global Navigation Satellite Systems) positioning method that requires SSR (State Space Representation) corrections in order to provide solutions with an accuracy of centimetric level. The so-called RT-PPP (Real-time PPP) is possible thanks to real-time precise SSR products, for orbits and clocks, provided by IGS (International GNSS Service) and its associate analysis centers such as CNES (Centre National d'Etudes Spatiales). CNES SSR products also enable RT-PPP with integer ambiguity resolution. In GNSS related literature, PPP with ambiguity resolution (PPP-AR) in real-time is often referred as PPP-RTK (PPP – Real Time Kinematic). PPP-WIZARD (PPP - With Integer and Zero-difference Ambiguity Resolution Demonstrator) is a software that is made available by CNES. This software is capable of performing PPP-RTK. It estimates slant ionospheric delays and other GNSS positioning parameters. Since ionospheric effects are spatially correlated by GNSS data from active networks, it is possible to model and provide ionospheric delays for any position in the network coverage area. The prior knowledge ionospheric delays can reduce positioning convergence for PPP-RTK users. Real-time ionospheric models could benefit from highly precise ionospheric delays estimated in PPP-AR. In this study, we demonstrate that ionospheric delays obtained throughout PPP-AR estimation are actu ally ionospheric observables. Ionospheric observables are biased by an order of few meters caused by the receiver hardware biases. These biases prohibit the use of PPP-WIZARD ionospheric delays to produce ionospheric models. Receiver biases correction is essential to provide ionospheric delays while using PPP-AR based ionospheric observables. In this contribution, a method was implemented to estimate and mitigate receiver hardware biases influence on slant ionospheric observables from PPP-AR. In order to assess the proposed approach, PPP-AR data from 12 GNSS stations were processed over a two-month period (March and April 2018). A comparison between IGS ionospheric products and PPP-AR based ionospheric observables corrected for receiver biases, resulted in a mean of differences of −39 cm and 51 cm standard deviation. The results are consistent with the accuracy of the IGS ionospheric products, 2–8 TECU, considering that 1 TECU is ~16 cm in L1. In another analysis, a comparison of ionospheric delays from 5 pairs of short baselines GNSS stations found an agreement of 0.001 m in mean differences with 22 cm standard deviation after receiver biases were corrected. Therefore, the proposed solution is promising and could produce high quality (1–2 TECU) slant ionospheric delays. This product can be used in a large variety of modeling approaches, since ionospheric delays after correction are unbiased. These results indicate that the proposed strategy is promising, and could benefit applications that require accuracy of 1–2 TECU (~16–32 cm in L1).     

W波段FMCW SAR系统实现与试验

与C波段、X波段和Ka波段相比,W波段的调频连续波(FMCW)合成孔径雷达(SAR)系统因具有更高的分辨率,更易实现低功耗与小型化而备受关注。W波段波长短,因此该波段的FMCW SAR更适用于短距离成像。提出一种W波段FMCW SAR系统的设计方案,根据提出的系统方案与指标,实现W波段FMCW轨道SAR系统的样机研制。该系统分辨率可达5 cm。系统样机试验在上海交通大学的多功能船模拖拽水池完成。设置不同目标进行成像试验,最终得到多组有效试验数据,并基于改进的RD算法进行数据处理,得到理想的SAR图像。经分析可知,系统实际分辨率优于5 cm。试验结果证明了W波段FMCW SAR系统的可行性与有效性。     

去中心化时差频差直接定位方法

针对原始利用时差频差的直接定位(DPD)方法存在数据传输量和计算量大的瓶颈,提出了两种去中心化直接定位方法。第1种方法采用去中心化配对方案,只将各观测站截获信号在站间进行一次传输,将数据传输和计算分散到各观测站间并行计算互模糊函数(CAF),构造仅满足满秩条件的互模糊矩阵(CAM)。第2种方法根据推导的任意互模糊函数间关系公式,采用归约方式去中心化的在各观测站并行计算余下互模糊函数,补全互模糊矩阵。两种方法都降低了直接定位数据传输量,提高了计算效率。性能分析和仿真实验表明本文两种方法精度性能优于两步定位方法,在低信噪比时两种方法都可达到比较理想的精度性能,在高信噪比时第2种方法与原始直接定位方法的精度性能相当。     

IMPROVEMENT OF PHASE GRADIENT AUTOFOCUS ALGORITHM

ＩＭＰＲＯＶＥＭＥＮＴＯＦＰＨＡＳＥＧＲＡＤＩＥＮＴＡＵＴＯＦＯＣＵＳＡＬＧＯＲＩＴＨＭＬｉＬｉｗｅｉ（李立伟），ＭａｏＳｈｉｙｉ（毛士艺），ＡｓｉｆＲａｚａ，ＬｉｕＹｉｎｇ（刘莹）（ＤｅｐａｒｔｍｅｎｔｏｆＥｌｅｃｔｒｏｎｉｃＥｎｇｉｎｅｅｒｉｎｇ...     

Enhancing the ATIC charge resolution

The Advanced Thin Ionization Calorimeter (ATIC) experiment is designed to investigate the charge composition and energy spectra of primary cosmic rays over the energy range from about 10¹¹ to 10¹⁴ eV during Long Duration Balloon (LDB) flights from McMurdo, Antarctica. Currently, analysis from the ATIC-1 test flight and ATIC-2 science flight is underway and preparation for a second science flight is in progress. Charge identification of the incident cosmic ray is accomplished, primarily, by a pixilated Silicon Matrix detector located at the very top of the instrument. While it has been shown that the Silicon Matrix detector provides good charge identification even in the presence of electromagnetic shower backscatter from the calorimeter, the detector only measures the charge once. In this paper, we examine use of the top scintillator hodoscope detector to provide a second measure of the cosmic ray charge and, thus, improve the ATIC charge identification.     

Scientific requirements for future spatially resolved white-light and broad-band high-cadence observations of the Sun

Several important issues are open in the field of solar variability and they wait their solution which up to now was attempted using critical ground-based instrumentations. However, accurate photometric data are attainable only from space. New observational material should be collected with high enough spatial and spectral resolution, covering the whole visible range of the electromagnetic spectrum as well infrared and ultraviolet to reconstruct the total solar irradiance: (1) the absolute contributions of different small-scale structural entities of the solar atmosphere from the white light flares and from micro-flares are still poorly known; (2) we do not know the absolute contributions of different structural elements of the solar atmosphere to the long-term and to the cyclic variations of the solar irradiance, including features of the polar regions of the Sun; (3) the variations of the chromospheric magnetic network are still poorly evaluated; (4) only scarce information is available about the spectral variations of different small-scale features in the high photosphere. Variability of the Sun in white light can be studied with higher spectral, spatial and time resolution using space-born telescopes, which are more appropriate for this purpose than ground based observatories because of better seeing conditions, no interference of the terrestrial atmosphere and a more precise calibration procedure. Scientific requirements for such observations and the possible experimental tools proposed for their solution. Suggested solar studies have broader astrophysical importance.