China's Planning for Deep Space Exploration and Lunar Exploration before 2030

The current lunar exploration has changed from a single scientific exploration to science and resource utilization. On the basis of the previous lunar exploration, Chinese scientists and technical experts have proposed an overall plan to preliminarily build a lunar research station on the lunar South Pole by several missions before 2035, exploring of the moon, as well as the use of lunar platforms and in-site utilization of resources. In addition, China will also explore Mars, asteroids and Jupiter and its moons. This paper briefly introduces the ideas of Chinese scientists and technical experts on the lunar and deep space exploration.      

China's Lunar and Deep Space Exploration Program for the Next Decade (2020-2030)

China has carried out four unmanned missions to the Moon since it launched Chang'E-1, the first lunar orbiter in 2007. With the implementation of the Chang'E-5 mission this year, the three phases of the lunar exploration program, namely orbiting, landing and returning, have been completed. In the plan of follow-up unmanned lunar exploration missions, it is planned to establish an experimental lunar research station at the lunar south pole by 2030 through the implementation of several missions, laying a foundation for the establishment of practical lunar research station in the future. China successfully launched its first Mars probe on 23 July 2020, followed in future by an asteroid mission, second Mars mission, and a mission to explore Jupiter and its moons.      

Hydrogen cyanide polymers on comets.

The original presence on cometary nuclei of frozen volatiles such as methane, ammonia and water makes them ideal sites for the formation and condensed-phase polymerization of hydrogen cyanide. We propose that the non-volatile black crust of comet Halley consists largely of such polymers. Dust emanating from Halley's nucleus, contributing to the coma and tail, would also arise partly from these solids. Indeed, secondary species such as CN have been widely detected, as well as HCN itself and particles consisting only of H, C and N. Our continuing investigations suggest that the yellow-orange-brown-black polymers are of two types: ladder structures with conjugated -C=N- bonds, and polyamidines readily converted by water to polypeptides. These easily formed macromolecules could be major components of the dark matter observed on the giant planets Jupiter and Saturn, as well as on outer solar system bodies such as asteroids, moons and other comets. Implications for prebiotic chemistry are profound. Primitive Earth may have been covered by HCN polymers either through cometary bombardment or by terrestrial happenings of the kind that brought about the black crust of Halley. The resulting proteinaceous matrix could have promoted the molecular interactions leading to the emergence of life.     

Radiation analysis for manned missions to the Jupiter system.

An analysis for manned missions targeted to the Jovian system has been performed in the framework of the NASA RASC (Revolutionary Aerospace Systems Concepts) program on Human Exploration beyond Mars. The missions were targeted to the Jupiter satellite Callisto. The mission analysis has been divided into three main phases, namely the interplanetary cruise, the Jupiter orbital insertion, and the surface landing and exploration phases. The interplanetary phase is based on departure from the Earth-Moon L1 point. Interplanetary trajectories based on the use of different propulsion systems have been considered, with resulting overall cruise phase duration varying between two and five years. The Jupiter-approach and the orbital insertion trajectories are considered in detail, with the spacecraft crossing the Jupiter radiation belts and staying around the landing target. In the surface exploration phase the stay on the Callisto surface is considered. The satellite surface composition has been modeled based on the most recent results from the GALILEO spacecraft. In the transport computations the surface backscattering has been duly taken into account. Particle transport has been performed with the HZETRN heavy ion code for hadrons and with an in-house developed transport code for electrons and bremsstrahlung photons. The obtained doses have been compared to dose exposure limits.     

Current review of the Jupiter, Saturn, and Uranus ionospheres

The ionospheres of the major planets Jupiter, Saturn, and Uranus are reviewed in light of Pioneer and Voyager observations. Some refinements to pre-Voyager theoretical models are required to explain the results, most notably the addition of significant particle ionization from ‛electroglow” and auroral processes and the need for additional chemical loss of protons via charge exchange reactions with water. Water from the Saturn rings has been identified as a major modifier of the Saturn ionosphere and water influx from satellites and/or meteorites may also be important at Jupiter and Uranus as well, as evidenced by the observed ionospheric structure and the identification of cold stratospheric carbon monoxide at Jupiter.     

模糊AHP法在雷达组网效能评估中的应用

由于雷达系统组网效能评估和优选工作涉及多个指标和大量的模糊属性,导致了决策工作的困难.把拓展的模糊层次分析方法AHP(Analytic Hierarchy Process)引入雷达组网系统效能评估领域,提出了组网雷达作战效能评价指标层次,根据区间数判断矩阵的有关概念,得到了区间数判断矩阵排序权向量或综合评价值的计算方法,利用概率分布法对各最底层元素关于最高层准则的总组合权重进行排序.应用基于区间模糊数判断矩阵的模糊AHP法,建立了模糊评判模型.实例分析结果表明该方法具有实用性,其评估结果可以辅助指挥员提高雷达组网布防决策的准确性和科学性.      

一种基于纯天文观测的火星车自主导航方法

提出了一种基于纯天文观测的火星车自主天文导航新方法.该方法仅需利用由星敏感器视场内测量得到的火星卫星(火卫一、火卫二)和某一恒星之间的星光角距,结合火星车的运动模型,通过Unscented粒子滤波方法,即可获得高精度的火星车实时位置信息.计算机仿真结果表明了该方法的有效性,同时对几个关键的精度影响因素进行了仿真分析.      

JUXTA: A new probe of X-ray emission from the Jupiter system

For the future Japanese exploration mission of the Jupiter’s magnetosphere (JMO: Jupiter Magnetospheric Orbiter), a unique instrument named JUXTA (Jupiter X-ray Telescope Array) is being developed. It aims at the first in-situ measurement of X-ray emission associated with Jupiter and its neighborhood. Recent observations with Earth-orbiting satellites have revealed various X-ray emission from the Jupiter system. X-ray sources include Jupiter’s aurorae, disk emission, inner radiation belts, the Galilean satellites and the Io plasma torus. X-ray imaging spectroscopy can be a new probe to reveal rotationally driven activities, particle acceleration and Jupiter–satellite binary system. JUXTA is composed of an ultra-light weight X-ray telescope based on micromachining technology and a radiation-hard semiconductor pixel detector. It covers 0.3–2 keV with the energy resolution of <100 eV at 0.6 keV. Because of proximity to Jupiter (∼30 Jovian radii at periapsis), the image resolution of <5 arcmin and the on-axis effective area of >3 cm² at 0.6 keV allow extremely high photon statistics and high resolution observations.     

China's Future Missions for Deep Space Exploration and Exoplanet Space Survey by 2030

Four future missions for deep space exploration and future space-based exoplanet surveys on habitable planets by 2030 are scheduled to be launched. Two Mars exploration missions are designed to investigate geological structure, the material on Martian surface, and retrieve returned samples. The asteroids and main belt comet exploration is expected to explore two objects within 10 years. The small-body mission will aim to land on the asteroid and get samples return to Earth. The basic physical characteristics of the two objects will be obtained through the mission. The exploration of Jupiter system will characterize the environment of Jupiter and the four largest Moons and understand the atmosphere of Jupiter. In addition, we further introduce two space-based exoplanet survey by 2030, Miyin Program and Closeby Habitable Exoplanet Survey (CHES Mission). Miyin program aims to detect habitable exoplanets using interferometry, while CHES mission expects to discover habitable exoplanets orbiting FGK stars within 10 pc through astrometry. The above-mentioned missions are positively to achieve breakthroughs in the field of planetary science.      

The meteorology of Jupiter's atmosphere

Observations of the atmosphere of Jupiter by the imaging and infrared instruments on the Voyager spacecraft have been analysed to provide new insight into the meteorology of Jupiter. Like the Earth, the atmosphere of Jupiter appears to behave in a quasi-geostrophic manner. For a period prior to the Voyager 1 encounter, the analysis on imaging data indicated that the eddy momentum transfer into the mean zonal flow was a major driving mechanism for the motions. The jet structures are a barotropic phenomena, which the large scale belts and zones depend on for the baroclinicity of the motions and form a family of features. The initial analysis shows that the meteorologies of the Earth and Jupiter have more in common than was previously thought.     

Using S-band dual polarized radar for convective/stratiform rain indexing and the correspondence with AMSR-E GSFC profiling algorithm

The separation of rain types in convective and stratiform regimes has long been a goal in microwave remote sensing of precipitation research. In this essence, a dual polarized radar based indexing scheme that provides information on convective and stratiform (C/S) rain regimes has been presented in correspondence with advanced microwave scanning radiometer – earth observing system (AMSR-E) GSFC profiling algorithm estimate of convective rain percentage. The dual polarized radar based C/S indexing scheme first retrieves the normalized gamma drop size distribution parameters, median volume drop diameter (D₀) and concentration parameter (N_w), from dual polarized radar measurements Z_H and Z_DR, representing reflectivity and differential reflectivity respectively, by means of the genetic programming approach. Next, the C/S rain index is calculated based on the formulation of an empirical relation in N_w–D₀ domain. The scheme has been inspected and applied on measurements from the S-band Chilbolton dual polarized radar. A considerable number of “coincident” cases from the radar and the AMSR-E observations are investigated. It has been revealed that the dual polarized radar based C/S rain indexing is in a similar pattern with the AMSR-E GSFC profiling algorithm estimate of convective rain percentage. Generally, as C/S rain index value increases, which signifies a stratiform to convective trend, the AMSR-E convective rain percentage also increases.     

距离门信号级的机载双基雷达地杂波模拟方法

由于几何配置的多样性,双基雷达地杂波模拟比较复杂.虽然单基雷达杂波散射元划分的方法可用于双基地杂波仿真,但不利于特定距离门信号的分析.在比较了单双基地雷达地面散射元等距线的基础上,提出一种距离门信号级的机载双基雷达地杂波模拟方法,距离向以双程斜距分辨率划分椭圆环,推导出地面椭圆表达式和散射元坐标解析解,方位向引入椭圆中间参量,在保证多普勒分辨率基础上划分杂波元网格,给出杂波模拟中未知参量的计算.该方法不仅能进行所有观测区域杂波功率谱的仿真,且可完成某些或某个距离门杂波回波信号的计算分析,实现距离门信号级杂波的模拟.仿真结果验证了该方法的有效性.      

基于IFA-HFS的雷达波形域LPI性能评估方法

针对雷达波形域低截获（LPI）性能评估的问题，提出一种应用改进萤火虫算法（IFA）求解指标权重的犹豫模糊集（HFS）评估方法。首先，介绍基于逼近理想解排序（TOPSIS）的犹豫模糊集理论，并从属性和方案2个角度构建指标权重的优化模型；其次，通过引入混沌理论，解决了萤火虫算法容易陷入局部最优的问题，给出用IFA求解指标权重的流程；再次，从雷达发射方角度，提取脉内、脉间5个波形域LPI性能评估指标；最后，得到利用IFA求解指标权重的犹豫模糊集评估方法。选取4种不同类型的雷达进行仿真对比，获得波形域LPI性能排序，验证了方法的快速性和有效性。      

基于不同角域RCS均值的雷达探测模型

针对目标在不同方位角的雷达散射截面积(RCS,Radar Cross Section)差异较大的情况,提出了一种基于目标不同角域内RCS均值的单部雷达探测概率模型及雷达网综合探测概率模型.计算机仿真平台中采用了两套不同的RCS取值方案:取单个RCS均值;根据探测方位角取不同角域内的RCS均值.两套方案所得探测概率差异表明:该模型符合雷达从不同方位角探测到目标的RCS差异较大的实际情况,计算所得探测概率更为精确.      

Statistical study of energetic electrons in Jupiter’s inner magnetosphere by Juno/JEDI

The Juno spacecraft made the first in-situ observations of energetic particles in the polar region of Jupiter’s magnetosphere. After Jupiter Orbit Insertion (JOI) in July 2016, data from ~20 Juno perijoves (PJs) obtained by Juno/JEDI are accumulated, providing an excellent opportunity to study the long term spatio-temporal distribution of energetic particles in Jupiter’s radiation belt. We transform Juno’s position from a Cartesian to a magnetic coordinate system by tracing magnetic field lines based on a fourth order Runge-Kutta method. Then the fluxes of energetic electrons from PJ1 to PJ14 sorted by different locations in magnetic coordinate space and the data are well organized by the L-shell parameter. The variation of electron flux increases with L-shell. The deviation (the ratio of the 75th percentile to the 25th percentile) of 0.51 MeV electron flux varies from a factor of 1.23 near L = 9.5 to 27.57 near L = 15.5. However, the mean flux decreases by about one order of magnitude in the same region. The electron spectra at larger L-shells are softer than that at smaller L-shells. On the other hand, the electron flux decreases more rapidly with increased L-shell when the location is off the equator. Along an L-shell, the electron flux decrease at first and then increase again from equator to mid-latitude region. In addition, we compare the statistical results with the widely used GIRE2 model. JEDI data correspond well with the GIRE2 model when the L-shell is > 14.75. GIRE2 underestimate the electron flux for L-shell smaller than 13.25. These results of this analysis are applicable to estimate the effects of the radiation environment in Jupiter’s magnetosphere.     

反导预警相控阵雷达网目标分配方法

针对相控阵雷达网跟踪弹道导弹目标时的资源管理问题，分析阐述反导预警作战场景，提出综合目标跟踪精度和雷达切换频率的目标分配效益函数，从雷达能量、时间及雷达与目标可见性三方面建立约束条件，以准确反映目标分配过程中的实际限制，在此基础上构建反导预警相控阵雷达网目标分配模型。根据反导预警任务特点，设置目标分配的自适应间隔，以提高模型设计合理性。就稀疏弹道导弹目标跟踪、密集弹道导弹目标跟踪2种场景进行仿真实验，结果表明:运用所提方法能够有效实现目标分配，提升相控阵雷达网资源利用效率，并能够减少雷达切换次数。      

Hydrogen cyanide polymers from the impact of comet P/Shoemaker-Levy 9 on Jupiter.

Hydrogen cyanide polymers--heterogeneous solids ranging in color from yellow to orange to brown to black--may be among the organic macromolecules most readily formed within the Solar System. The non-volatile black crust of comet Halley, for example, as well as the extensive orange-brown streaks in the atmosphere of Jupiter, might consist largely of such polymers synthesized from HCN formed by photolysis of methane and ammonia. Laboratory studies of these ubiquitous compounds point to the presence of polyamidine structures synthesized directly from hydrogen cyanide. These would be converted by water to polypeptides which can be further hydrolyzed to alpha-amino acids. Other polymers and multimers with ladder structures derived from HCN would also be present and might well be the source of the many nitrogen heterocycles, adenine included, detected by thermochemolytic analysis. The dark brown color arising from the impacts of comet P/Shoemaker-Levy 9 on Jupiter could therefore be mainly caused by the presence of HCN polymers, whether originally present, deposited by the impactor or synthesized from freshly formed HCN. Spectroscopic detection of these predicted macromolecules and their hydrolytic and pyrolytic by-products would strengthen significantly the hypothesis that cyanide polymerization is a preferred pathway for prebiotic and extraterrestrial chemistry.     

基于CEEMDAN的雷达信号脉内细微特征提取法

有效的信号特征提取是高精度雷达辐射源识别的基础,以脉冲描述字为代表的传统特征已无法满足复杂电磁环境的需要。本文提出一种基于自适应噪声完备集合经验模态分解（CEEMDAN）的有效雷达辐射源脉内细微特征提取算法。雷达信号由对非平稳、非线性信号尤为有效的CEEMDAN分解产生的个别分量重构,抑噪效果通过1 000次蒙特卡罗实验得到验证,同时设计基于该重构的一种脉内特征空间。本文方法与主流特征提取方法的识别精度在6部雷达辐射源产生的3 000个不同脉内调制的加噪信号样本上进行了实验对比,结果表明不同种类信号样本在本文特征空间中清晰可分,本文方法较之主流方法更加精确,尤其在0 dB信噪比（SNR）下仍保持90%以上的高精度。      

ADS与多雷达数据融合中的系统误差配准法

对空中交通管制中自动相关监视(ADS)与现有多雷达监视系统进行数据融合的模型进行了分析,在现有多雷达数据处理(MRDP)系统误差配准方法的基础上设计了一种利用最小平方估计(LSE)准则实现的ADS与雷达的系统误差配准算法,给出了其最优解.利用我国西部航路模拟航路点数据进行了系统仿真,仿真结果的分析表明,通过该方法的配准,ADS和雷达数据融合中的系统误差得到了有效的消除,提高了综合监视精度.     

Shoemaker－Levy9彗星撞击木星的流星物理学

本文从流星物理学的基本方程出发,导出Shoemaker-Levy9慧星撞击木星时的速度、质量损失、电子线密度、能量释放率随高度的分布公式;采用合理的参数,作了一系列计算,并与观测资料比较,进行一些讨论。