导航卫星非差精密定轨测站选取策略分析

推导了测站分布对定轨精度影响的公式,提出一种兼顾测站数量、观测数据质量以及测站地理分布的测站选取策略。利用IGS和iGMAS全球观测网数据,设计了3种不同的测站分布方案,进行GPS精密定轨实验。结果表明,使用30个全球均匀分布的测站,GPS三维定轨精度能达到6.0 cm左右|使用40个全球均匀分布的测站,GPS三维定轨精度能达到3.5 cm的水平|使用50个全球均匀分布的测站,GPS三维定轨精度能达到2.8 cm以内|超过50个的测站对GPS定轨精度提高基本上没有贡献。     

基于CSST多色测光的时序测光精度分析

中国巡天空间望远镜(Chinese Survey Space Telescope, CSST)是中国的首个大型空间光学望远镜, 将对包括系外行星探测在内的诸多科学目标开展研究, 有望取得前沿科学进展. 时序测光精度是CSST重要的性能指标, 受到物理噪声和仪器噪声的影响, 需要通过数值模拟对其分析和评估. 模拟基于目前公布的CSST主要技术参数, 建立了时序的恒星信号和噪声模型, 以CSST的i波段为例, 分析凝视观测模式下的测光精度. 通过数值仿真, 展示了孔径测光中各项噪声的贡献, 特别是由指向抖动和像素响应不均匀性导致的抖动噪声. 模拟结果还给出了测光孔径的推荐范围. 为了获得更高的信噪比, 可以减小仪器抖动振幅和像素不均匀性, 或者采用参考星较差测光的方式. 结果为CSST后续的时序测光精度与不同指标参数的相关性分析、系外行星探测能力评估以及测光数据处理提供了模拟数据的支撑.     

国产高分系列卫星在森林火灾应急处置中的全流程应用——以四川九龙县三岩龙乡“4·08”森林火灾为例

四川西部高山峡谷地貌发育,山高林密且地质环境恶劣,区内林草资源丰富,森林火灾多发、易发、频发,灾害应急处置难度大,防控任务重。国产高分系列卫星影像具有时空分辨率高、载荷类型多、机动性强、幅宽范围大、成像迅速等优点,对川西地区森林防灭火、灾害应急处置及防灾减灾等有明显优势。以2021年四川九龙县三岩龙乡“4·08”森林火灾为例,利用国产高分系列卫星数据分别对森林火灾初期、中期及晚期开展应急处置,包括快速解译林火火灾救援要素(初期)、感知亮温异常态势(中期)、跟踪监测过火区动态(中期)、结合火场需求提供应急扑救部署建议(中期)、开展灾损解译评估(晚期)及火后泥石流易发性评价(火后)等,结果表明国产高分系列卫星对森林火灾应急处置的全流程应用具有实践指导意义。     

精密单点定位估计GPS卫星的P1-C1码偏差及稳定性分析

给出了利用精密单点定位（PPP）技术估计GPS卫星P1-C1码偏差的数学模型,并以BRUS、GODE、SHAO和NIST四个跟踪站2010年10月份一个月的观测数据为例,采用PPP方法计算了所有GPS卫星的P1-C1码偏差,并与欧洲定轨中心提供的P1-C1码偏差进行了比较,结果表明：四个站估计的P1-C1码偏差精度均可达到几个厘米。一个月的计算结果表明：卫星的P1-C1码偏差在一个月内变化平缓。     

卫星编队InSAR系统分辨率设计

依据脉冲信号压缩技术,从SAR成像理论出发,在介绍了SAR分辨率定义的基础上,分析了影响基于卫星编队InSAR系统分辨率的原因是存在距离向和方位向基线。在成像处理时,为了确保干涉相位精度,需进行去相关预滤波处理,由此引起系统成像带宽变窄,分辨率下降。依据影响分辨率的原因,提出了基于卫星编队InSAR系统分辨率设计思想,并根据该思想对分辨率的影响情况进行了分析。     

Trajectory Analysis and Design for A Jupiter Exploration Mission

The trajectory design for a Jupiter exploration mission is investigated in this paper. The differences between the Jupiter exploration trajectory and the Mars or Venus exploration trajectory are mainly concerned about. Firstly, the selection of the Jupiter-centered orbit is analyzed based on the Galileo Jupiter mission. As for the Earth-Jupiter transfer orbit, the fuel consumption of the direct transfer is too large. So the energy-saving technologies such as the planetary gravity assist should be used for the trajectory to the Jupiter. The different sequences of planetary gravity assists are examined by applying the Particle Swarm Optimization (PSO). According to the searched result, the Venus-Earth-Earth sequence (VEEGA) is the most effective one for the Jupiter mission. During the Jupiter mission, the spacecraft will pass though the main asteroid belt between the orbits of Mars and Jupiter, and may encounter multiple asteroids. Therefore the Jupiter mission is able to combine with the main-belt asteroid flyby mission. The design method of the intermediate asteroid flyby trajectory is also considered. At last, an entire trajectory for the Jupiter mission launched in 2023 is presented.     

太阳风在地球激波前兆区减速的统计研究

本文首次利用完全相同两颗卫星（CLUSTER C1和C3）的数据对地球激波前兆区太阳风的减速和偏转特性进行了统计研究.结果表明,在激波前兆坐标系中,太阳风减小的速度随观测点到激波的距离D_BS增大而减小,随行星际磁场与激波法向夹角θ_BN增大也减小,在ULF波动区深度D_WS小于6R_e(R_e为地球半径)的范围内最为显著;伴随着太阳风减速的另外一个现象——太阳风的偏转,也存在相似的规律.其最大减速和最大偏转角度分别为10 km/s和3°.太阳风减速和偏转,以及随之变化的太阳风动压,可能会引起地球磁层顶位置和形状发生改变,同时也为激波前兆区弥散（diffuse）离子的起源及加热提供了一种可能的机制.     

On the migration of a system of protoplanets

The evolution of a system consisting of a protoplanetary disc with two embedded Jupiter-sized planets is studied numerically. The disc is assumed to be flat and non-self-gravitating; this is modelled by the planar (two-dimensional) Navier–Stokes equations. The mutual gravitational interaction of the planets and the star, and the gravitational torques of the disc acting on the planets and the central star are included. The planets have an initial mass of one Jupiter mass M _Jup each, and the radial distances from the star are one and two semimajor axes of Jupiter, respectively.
During the evolution a joint wide annular gap is created by the planets. Both planets increase their mass owing to accretion of gas from the disc: after about 2500 orbital periods of the inner planet it has reached a mass of 2.3  M _Jup, while the outer planet has reached a mass of 3.2  M _Jup. The net gravitational torques exerted by the disc on the planets result in an inward migration of the outer planet on time-scales comparable to the viscous evolution time of the disc. The semimajor axis of the inner planet remains constant as there is very little gas left in its vicinity to induce any migration. When the distance of close approach eventually becomes smaller than the mutual Hill radius, the eccentricities increase strongly and the system may become unstable.
If disc depletion occurs rapidly enough before the planets come too close to each other, a stable system similar to our own Solar system may remain. Otherwise the orbits may become unstable and produce systems like υ And.     

The evolution of bodies orbiting in the trans-Neptunian region on to intermediate-type orbits

We investigate the dynamical evolution of 210 hypothetical massless bodies initially situated between 10 and 30 au from the Sun in order to determine the general characteristics of the evolved system. This is of particular relevance to the understanding of the origin of Edgeworth–Kuiper belt objects on scattered intermediate orbits, such as 1996 TL ₆₆, which have high eccentricity and semimajor axis but nevertheless have perihelion in the region between 30 and 50 au from the Sun.