Analysis of Theories of Fully Ionized Space Plasma

The physical sense of the main ideas, presently used in plasma physics, is discussed. An attempt is made to clarify the concepts, used in plasma physical calculations. The concept of `Coulomb collisions' with the implicitly introduced rapid stochastization plays the main negative role in the physics of fully ionized plasma. Statistical methods, which are adequate for the neutral gas and for the partially ionized plasma, are not applicable for the completely ionized case. It is the cause of large errors in evaluating real plasma parameters. A new concept is considered: a fully ionized space plasma should be treated as a dynamical system with a low level of chaos. Further progress in space physics requires a serious renewal of plasma theory.     

多输入多输出雷达的非均匀线性阵列配置(英文)

提出了利用非均匀线性阵列(Non-uniform linear array,NLA)对多输入多输出(Multiple-input multipleoutput,MIMO)雷达系统进行阵列配置优化的方法。在传统的相控阵雷达中,非均匀线性阵列配置被用来形成较窄的波束方向图,而在MIMO雷达中,利用非均匀线性阵列来获得更多的互不相同的虚拟阵元,以此来提高雷达的参数可辨识性能。文中所采用的一种非均匀线性阵列是最小冗余线性阵列,并给出了一种在物理阵元数量较大时最小冗余线性阵列的生成方法。实验结果表明:与均匀线性阵列(Uniform linear array,ULA)配置的MIMO雷达相比,非均匀线性阵列MIMO雷达能够利用较少的物理天线阵元获得相同的参数可辨识性能;而在两种配置的雷达系统的物理阵元个数相同的情况下,非均匀线性阵列MIMO雷达可以获得更大的阵列孔径长度和更低的克拉美.罗界。     

空间绕飞航天器间电磁兼容仿真分析方法

研究了空间绕飞任务中主、从航天器之间的电磁干扰问题,提出了绕飞过程中航天器间电磁兼容仿真分析方法。根据主、从航天器天线的发射功率、带外抑制、接收机灵敏度的信息,解算出了发射天线对接收天线的等效干扰。在假定计算模型作为仿真输入的前提下,得到了航天器间电磁兼容分析结果。仿真结果表明,所提出的仿真分析方法能够对绕飞任务中航天器间的电磁干扰进行预测,可为实际任务的顺利完成提供技术支持。     

变速变姿态下飞机燃油体积解算技术

为准确测量飞机不规则油箱内的燃油体积,在传统的查表插值法基础上,提出了基于等效传感器的自适应步长切割法（ASCM）,用于建立燃油质量特性数据库,通过引入等效传感器概念,实现了不同姿态下多传感器的信息融合;该方法根据切片截面积的变化率调整切割步长,从而减小了燃油体积解算时的插值误差;利用多传感器的输出值实现了燃油平面的最小二乘（LMS）拟合,当有效传感器较少时,再结合等效燃油平面姿态角拟合燃油平面,消除了加速度对燃油平面的影响;对传统的三维查表插值法进行改进,减小了由于燃油平面姿态角插值引起的误差。基于UG二次开发,设计了燃油体积解算平台。实际油箱CAD仿真验证结果表明:该方法所建的数据库数据规模小,燃油解算速度快,实现了加速度和姿态误差修正,并减小了差值误差,进一步提高了燃油的测量精度。      

The Rotation and Interior Structure Experiment on the InSight Mission to Mars

The Rotation and Interior Structure Experiment (RISE) on-board the InSight mission will use the lander’s X-band (8 GHz) radio system in combination with tracking stations of the NASA Deep Space Network (DSN) to determine the rotation of Mars. RISE will measure the nutation of the Martian spin axis, detecting for the first time the effect of the liquid core of Mars and providing in turn new constraints on the core radius and density. RISE will also measure changes in the rotation rate of Mars on seasonal time-scales thereby constraining the atmospheric angular momentum budget. Finally, RISE will provide a superb tie between the cartographic and inertial reference frames. This paper describes the RISE scientific objectives and measurements, and provides the expected results of the experiment.     

Presolar Isotopic Signatures in Meteorites and Comets: New Insights from the Rosetta Mission to Comet 67P/Churyumov–Gerasimenko

Comets are considered the most primitive planetary bodies in our Solar System, i.e., they should have best preserved the solid components of the matter from which our Solar System formed. ESA’s recent Rosetta mission to Jupiter family comet 67P/Churyumov–Gerasimenko (67P/CG) has provided a wealth of isotope data which expanded the existing data sets on isotopic compositions of comets considerably. In this paper we review our current knowledge on the isotopic compositions of H, C, N, O, Si, S, Ar, and Xe in primitive Solar System materials studied in terrestrial laboratories and how the Rosetta data acquired with the ROSINA (Rosetta Orbiter Sensor for Ion and Neutral Analysis) and COSIMA (COmetary Secondary Ion Mass Analyzer) mass spectrometer fit into this picture. The H, Si, S, and Xe isotope data of comet 67P/CG suggest that this comet might be particularly primitive and might have preserved large amounts of unprocessed presolar matter. We address the question whether the refractory Si component of 67P/CG contains a presolar isotopic fingerprint from a nearby Type II supernova (SN) and discuss to which extent C and O isotope anomalies originating from presolar grains should be observable in dust from 67P/CG. Finally, we explore whether the isotopic fingerprint of a potential late SN contribution to the formation site of 67P/CG in the solar nebula can be seen in the volatile component of 67P/CG.     

Dust Evolution in Protoplanetary Discs and the Formation of Planetesimals

After 25 years of laboratory research on protoplanetary dust agglomeration, a consistent picture of the various processes that involve colliding dust aggregates has emerged. Besides sticking, bouncing and fragmentation, other effects, like, e.g., erosion or mass transfer, have now been extensively studied. Coagulation simulations consistently show that \(\upmu\mbox{m}\)-sized dust grains can grow to mm- to cm-sized aggregates before they encounter the bouncing barrier, whereas sub-\(\upmu\mbox{m}\)-sized water-ice particles can directly grow to planetesimal sizes. For siliceous materials, other processes have to be responsible for turning the dust aggregates into planetesimals. In this article, these processes are discussed, the physical properties of the emerging dusty or icy planetesimals are presented and compared to empirical evidence from within and without the Solar System. In conclusion, the formation of planetesimals by a gravitational collapse of dust “pebbles” seems the most likely.