2021年宇航领域科学问题和技术难题在中国航天大会发布

正在以"新起点新征程新愿景"为主题的2021年中国航天大会上,中国宇航学会发布2021年宇航领域科学问题和技术难题。1.太阳磁场周期性反转与太阳全球磁场探测太阳活动周期本质上是由太阳磁场的周期性反转引起的,太阳磁场问题进一步制约着太阳物理学科的发展。缺乏观测数据是问题难以解决的关键,需要太阳物理和现代航天技术相结合,打开突破的大门。2.星系生态环境中的反馈效应及"重子缺失"问题在星系演化过程中存在着超新星爆发或黑洞喷流对环境的反馈效应,由于缺乏观测手段,其物理过程仍不确知。     

2021年宇航领域科学问题和技术难题在中国航天大会发布

正在以"新起点新征程新愿景"为主题的2021年中国航天大会上,中国宇航学会发布2021年宇航领域科学问题和技术难题。1.太阳磁场周期性反转与太阳全球磁场探测太阳活动周期本质上是由太阳磁场的周期性反转引起的,太阳磁场问题进一步制约着太阳物理学科的发展。缺乏观测数据是问题难以解决的关键,需要太阳物理和现代航天技术相结合,打开突破的大门。2.星系生态环境中的反馈效应及"重子缺失"问题在星系演化过程中存在着超新星爆发或黑洞喷流对环境的反馈效应,由于缺乏观测手段,其物理过程仍不确知。     

日地L4/L5点太阳立体探测任务初步设计

太阳耀斑和日冕物质抛射不仅是太阳物理研究中的重要课题，也是空间环境探测研究的重要对象。文章提出了一种在日地L4/L5点布置一颗探测器开展太阳立体探测的技术构想，相较于目前国际上在地球轨道或日地L1点布置探测器只能沿日地连线方向获取正对地球的太阳活动信息而言，该构想具有更大的优势，能够从侧面对整个日地连线上的日冕物质传播和演化规律进行立体监测，获取单点探测无法得到的立体信息，从而大大丰富太阳磁场、太阳活动等信息。文章在国外相关任务调研的基础上，对达到L5点的轨道转移方式和代价进行了初步计算，提出了探测器总体方案设想，并对我国开展L4/L5点太阳立体探测给出了未来发展建议。     

我国将研制天文卫星

本刊讯“将太阳望远镜送到大气层外的太空”这一创举将由中国空间技术研究院与中国科学院及下属的北京天文观测中心联手实现。这是从中国空间技术研究院最近召开的空间太阳望远镜先期启动动员会上传来的消息。 空间太阳望远镜属空间天文卫星。卫星的主要任务是将太阳望远镜送到大气层外的太空，在广泛的光谱范围和连续的时间演化上，通过高空间分辨率、高时间分辨率太阳探测，实现太阳物理研究的重大突破，并为空间天气预报提供重要依据和新方法。卫星投入使用后，由于它所利用的我国首创的光谱仪和超高空间分辨率技术，其提供的探测成果，…     

日发射太阳研究卫星

日本M-5固体火箭9月23日在内之浦航天中心发射了“太阳”B（又称“日出”）卫星以及“北海道工业大学星”（HITSAT）1和“太阳帆子有效载荷卫星”（SSSat）2两颗微小卫星。“太阳”B重870公斤，由三菱电气公司制造，将用于测量太阳磁场，以更好地认识影响地球的剧烈的太阳活动。星上载有与美、英联合研制的光学、红外和紫外望远镜各一台，能对太阳磁场进行迄今最近距离的观测。它将在太阳同步轨道上运行3年，其中3／4的时间处于阳光直接照射之下。     

基于PDM-MZM的线性模拟光链路设计

模拟光链路因其大带宽、低损耗等优势,在宽带无线通信、多基地雷达、卫星载荷信号馈送、电子战存储转发中极具应用前景，成为了当前微波光子领域研究的热点。然而由于电光调制和光电探测的非线性, 模拟光链路的动态范围受限。基于偏振复用马曾调制器的线性模拟光链路，通过改变两个RF信号的电功率比及两个子调制器的直流偏置点，可以分别改变调制指数比和光功率比，从而构造了两个相位相反的非线性失真信号以抵消链路的三阶交调失真，改善系统的无杂散动态范围。实验结果表明，与基于单个马曾调制器的常规链路相比，基于偏振复用马曾调制器的链路三阶交调失真被抑制33.7dB，无杂散动态范围提高17.6 dB，宽带射频信号的星座图和误差矢量幅度改善明显。     

一种新型的高精度偏振调制技术

文章提出一种新型的偏振调制技术--光谱调制,它能够获取目标的全部线偏振信息,其优势是体积小、质量轻、无运动部件、解调算法简单、解调精度高,特别适用于星载大气探测类载荷。该调制方法中入射的偏振光经过光谱调制偏振测量模块后,被调制为振幅随着线偏振度变化而相位随着线偏振角变化的正弦曲线,经算法解调,能够直接得到目标的线偏振度及线偏振角信息,而传统的偏振调制方法需要得到斯托克斯（Stokes）矢量的 I、Q、U、V 四个参量后经进一步计算才可以得到。文章对光谱调制偏振测量技术进行了理论与仿真分析,分析结果表明了该技术在理论上的可行性。     

深空探测激光通信技术发展研究

对美国深空探测活动中应用的激光通信技术进行了总结,说明当前深空光端机正向着更加集成化、轻型化和多功能化的方向发展;重点对深空激光通信中的捕获跟踪瞄准、接收和调制等关键技术进行了分析;针对中国激光通信的发展和应用提出了建议,如突破激光器和高速率调制器等关键技术,深入研究新型编码算法等。     

矢量调制器在星载相控阵天线中的应用

精确的相位调制技术是星载毫米波有源相控阵天线最关键技术之一。传统的数字移相器构造较为复杂,尺寸较大,相位调制特性有局限性,不是高工作频段、宽扫描角星载相控阵天线发展的最优选择。文章提出采用单片矢量调制器来代替数字移相器及数字衰减器,利用电压来控制矢量调制器的相位调制,提高了相位调制性能,同时具有结构简单、尺寸较小等优点。在此基础上设计了星载毫米波段有源相控阵天线,并且实现了精确的二维波束扫描功能,验证了矢量调制器在星载毫米波有源相控阵天线中应用的技术可行性。     

空间能量粒子探测方法研究

阐述了空间能量粒子探测的原理和方法。介绍了国外在能量粒子探测方面所采用的半导体望远镜测量法、电场加速法、磁偏转法等方法，分析了它们各自的优缺点。就制约能量粒子探测技术发展的关键因素进行了讨论。并以此为基础，结合我国实际情况提出了一种新的探测方法。     

Alfven modes of solar coronal magnetic arches: Excitation of ballooning instability and modulation of flare emission

The effect of Alfven-type oscillations in a coronal magnetic arch on modulation of the gyrosynchrotron radiation and development of the ballooning instability in the arch is considered. On the basis of the energy method and the method of normal modes, the expressions are obtained for increments of ballooning instability at its swinging by natural oscillations of the arch. The conclusion is drawn that bending oscillations, which do not actually compress the plasma and, therefore, represent the Alfven-type modes, unlike the radial oscillations, are capable, under solar corona conditions, to effectively swing ballooning instability and, as a consequence, play a part of a trigger for solar flares. The ballooning instability of coronal arches is shown to be capable of causing formation of helmet-shaped structures in the lower solar corona. On the basis of calculations of the intensity modulation depth and the degree of circular polarization of non-thermal gyrosynchrotron radiation, under the assumption of excited Alfven oscillations of a coronal arch, the conclusion is drawn, that microwave observations at a frequency of > 10 GHz can be used for studying the conditions of excitation and propagation of Alfven modes in flare loops. The consequences of obtained results are discussed using the flare on April 15, 2002 as an example.     

Coronal mass ejections in July 2005 and an unusual heliospheric event

Using the events in July 2005 as an example, the causes and peculiarities of Forbush effects produced by solar sources remote from the central zone are discussed. The event in question differs from other effects observed at the periphery of interplanetary disturbances by strong variations in cosmic rays on the background of weak disturbances in the solar wind and magnetic field of the Earth. The cloud of magnetized plasma ejected from the Sun was large and fast, but it passed to the west from the Sun-Earth line. According to performed estimates, the mass of the ejected substance was close to the upper boundary of mass for coronal mass ejections (CMEs). Anomalous parameters and high modulation capability of the formed solar wind disturbance are explained, in particular, by the fact that it combined several CMEs and that the last fast disturbance was prepared by a series of impulsive events in the active region of the Sun. Usually, such a great mass is ejected directly after the main energy release in strong solar flares. In the given case, a powerful MHD disturbance occurred approximately half an hour after a maximum of hard X-ray burst under the conditions when gas pressure in the flare loops became close to magnetic pressure, which was just a premise of the largescale ejection.     

Vertical structure of the magnetic field in active regions of the sun at coronal heights

High-altitude measurements and magnetic field distribution in active regions are always an important problem to verify existing models at heights from units to hundreds of Mm. Optical methods of analysis of the magnetic structure work well only at the photosphere level. At the same time, the progress of radio astronomy methods of analyzing the solar radio emission [1] and of the theory of solar plasma radiation [2] facilitates introduction of new methods for measuring the magnetic field strength at various altitudes in the solar atmosphere. In this paper we use multi-wave observations of polarization of the radio emission of active regions in the microwave range together with precise magnetosphere data in order to develop a method of projection for measuring the height distribution of the magnetic field.     

基于被动探测的目标磁扰动信号检测与定位

针对目标探测定位的快速发展中,军事领域主动雷达存在的缺陷和实现具有高度隐蔽性的目标检测技术的需求,提出一种基于被动磁矢量测量的目标扰动信号检测与定位技术。该方法利用磁传感器阵列测量目标产生的磁矢量扰动信息,通过滤波、门限检测、基函数展开等技术将有效扰动从复杂的背景场中提取出来,并结合速度估计、磁梯度张量矩阵算法研究任意目标位置的定位技术。理论和仿真结果证明了所提出的信号检测与定位技术的正确性,实地测试结果表明该方法具有较高的可行性和实用潜质。     

一种Ka频段单通道调制器的设计与实现

随着航天事业的不断发展,卫星平台及有效载荷的轻量化、小型化是未来航天系统的发展趋势。单通道单脉冲跟踪系统在航天器中有着广泛的应用,而单通道调制器是单通道单脉冲跟踪系统的重要组成部分。为顺应星载自跟踪系统轻量化、小型化发展趋势,根据工程化要求,采用多芯片微组装技术,通过合理的系统分析和仿真设计,在厚度为0.254mm、相对介电常数为2.2的ROGERS 5880介质基板上设计实现了一种Ka频段单通道调制器。该调制器实现了小型化和集成化,采用BJ260波导作为输入,其和通道增益大于30dB,噪声系数优于2.5dB,载波抑制大于50dB,调制抑制大于30dB,经过地面各项试验及在轨飞行验证,其各项指标满足要求。     

Effect of large and sharp changes of solar wind dynamic pressure on the earths’s magnetosphere: analysis of several events

The magnetosphere and ionosphere response to arrival of large changes of the solar wind dynamic pressure with sharp fronts to the Earth is considered. It is shown that, under an effect of an impulse of solar wind pressure, the magnetic field at a geosynchronous orbit changes: it grows with increasing solar wind pressure and decreases, when the solar wind pressure drops. Energetic particle fluxes also change: on the dayside of the magnetosphere the fluxes grow with arrival of an impulse of solar wind dynamic pressure, and on the nightside the response of energetic particle fluxes depends on the interplanetary magnetic field (IMF) direction. Under the condition of negative Bz-component of the IMF on the nightside of the magnetosphere, injections of energetic electron fluxes can be observed. It is shown, that large and fast increase of solar wind pressure, accompanied by a weakly negative Bz-component of the IMF, can result in particless’ precipitation on the dayside of the auroral oval, and in the development of a pseudobreakup or substorm on the nightside of the oval. The auroral oval dynamics shows that after passage of an impulse of solar wind dynamic pressure the auroral activity weakens. In other words, the impulse of solar wind pressure in the presence of weakly negative IMF can not only cause the pseudobreakup/substorm development, but control this development as well.     

Motion and transport of solar cosmic rays in heliospheric traps: The event on January 28–31, 2001

The results of studying the enhancement of solar cosmic ray fluxes on January 28?C31, 2001 in a wide energy range are presented using the ACE spacecraft data. A comparative analysis of temporal variations of the fluxes of charged particles and of the interplanetary medium parameters (interplanetary magnetic field and solar wind) has been performed on the basis of the ??reflection?? model of motion, accumulation, and modulation of cosmic rays. It is shown that a magnetic trap for solar cosmic rays was created by a plasma stream and flare ejection from an active region in the western part of the solar disk. Particles of low energies (<10 MeV) were captured inside the trap; the dispersion of distribution of particles with different energies inside the trap being determined by its complicated magnetic structure. The power-low dependence of the time of maximum for the flux of particles on their energy is found, and softer energy spectrum inside the trap is explained.     

光学遥感图像船只目标检测识别技术

船只目标检测识别技术是现阶段遥感图像研究领域的一个重要发展方向。随着国产高分辨率卫星的快速发展，高分遥感卫星陆续发射，基于光学遥感图像的船只检测识别技术会逐步成为研究热门。主要介绍了近年来基于光学图片的船只检测识别技术发展、以及当前技术存在的问题。当前基于深度学习的船只目标检测识别技术取得了较好的检测效果，成为主流研究方向，但在光学遥感图像船只检测领域基于深度学习的方法有一些基本问题限制了检测效果，对这些问题进行了归纳总结，并对未来光学遥感图像船只检测技术的发展进行了展望。     

利用地磁场测量的小卫星自主导航设计

地磁场矢量是卫星所在位置的函数 ,通过对地磁场的测量 ,即可实现对近地小卫星的自主导航。本文采用卡尔曼滤波技术设计了小卫星基于地磁场测量的导航方法 ,在采用地磁场模型时选取磁偶极子模型 ,以此使设计算法的计算量大大减少。最后利用数字仿真验证了系统性能。