空间TDICCD相机动态信噪比计算方法研究

信噪比是空间光学相机系统的主要设计指标之一,可用于表征相机的辐射性能。文章通过建立遥感卫星轨道模型,分析计算一年中任意时刻用太阳高度角和卫星观测角描述太阳、卫星、地面目标点之间的相对位置关系,并将计算得到的卫星观测角和太阳高度角等参数导入大气传输软件MODTRAN,输出在相机入瞳处的地面目标光谱辐亮度,再根据信噪比的计算方法,最后完成TDICCD相机动态的信噪比计算值。通过该方法,可以计算任一时刻任一观测目标的信噪比,这将有利于判断在某一时刻的能量是否满足观测要求,以随时改变TDICCD的探测器级数,使得成像像质达到最佳。     

N中连续取k好可修系统的模糊可靠性

在假定关键部件具有较高的修理优先权的条件下,讨论了具有1个修理工的可修n中连续取k好系统.利用马尔可夫过程对系统的各状态进行分析,得出了系统各状态的概率.然后利用基于模糊状态的可靠性理论,通过定义系统各状态对模糊成功的隶属函数,得到了可修n中连续取k好系统的模糊可靠性指标的计算公式,并比较其结果与传统可靠性理论的不同之处.模糊可靠度可以反映系统中工作部件的数目对系统性能的影响,它全面刻画了系统的可靠性行为.最后给出了计算示例说明算法.     

圆轨道航天器八面体编队构型轨道动力学分析

提出一个全新的八面体航天器编队构型,该构型体现出当前编队飞行多种轨道构型的特征,同时也适于作为空间演示试验的编队飞行模式。八面体编队构型的设计思路是基于C-W方程,轨道平面内沿航向编队构型可利用轨道动力学自然保持,正上方或正下方编队构型则需要依靠平面内控制来实现,垂直轨道平面的编队构型需要施加法向控制来实现。对基于C-W方程的悬停动力学模型进行了精度分析,最后以低轨道航天器的八面体编队构型为例进行了数学仿真验证。     

卫星编队飞行的相对轨道自主确定研究

为了研究卫星编队飞行相对轨道的自主确定,基于相对轨道根数建立编队卫星间的相对运动方程,利用测量所得到的星间距离和方位信息作为观测量。不同于目前广泛采用的扩展卡尔曼滤波算法,设计Unscented Kalman Filter(UKF)算法实现卫星编队飞行的相对轨道自主确定。仿真结果表明这种相对轨道自主确定方案能获得较高的定轨精度。     

AVS-F observations of γ-ray emission during January 20, 2005 solar flare up to 140 MeV

The solar flare of January 20, 2005 (X7.1, 06:36–07:26 UT, maximum at 07:01 UT by the GOES soft X-ray data) was the most powerful one in January 2005 series. The AVS-F apparatus onboard CORONAS-F registered γ-emission during soft X-ray rising phase of this flare in two energy ranges of 0.1–20 MeV and 2–140 MeV. The highest γ-ray energy registered during this flare was ∼140 MeV. Six spectral features were registered in energy spectrum of this solar flare: annihilation + αα (0.4–0.6 MeV), ²⁴Mg + ²⁰Ne + ²⁸Si + neutron capture (1.7–2.3 MeV), ²¹Ne + ²²Ne + ¹⁶O + ¹²С (3.2–5.0 MeV), ¹⁶O (5.3–6.9 MeV), one from neutral pions decay (25–110 MeV) and one in energy band 15–21 MeV. Four of them contain typical for solar flares lines – annihilation, nuclear de-excitation and neutron capture at ¹H. Spectral feature caused by neutral pions decay was registered during several flares too. Some spectral peculiarities in the region of 15–21 MeV were first observed in solar flare energy spectrum.     

Ozone destruction by solar electrons in relation to solar variability and the terrestrial latitude

Precipitating electrons from the radiation belts with energies greater than from 150 keV to 5 MeV have been correlated with ozone data of a large number of stations located within 40–70° N. Energetic electrons have been collected by the low altitude polar Russian satellite METEOR while ozone data have been compiled from almost ninety (90) stations located all over the world within the latitude zone 40–70° N.     

Multi-objective output-feedback control for microsatellite attitude control: An LMI approach

Mixed H₂/H_∞ output-feedback controller with pole placement constraints against the internal uncertainty of moment-of-inertia variation and space environmental disturbances is proposed for mircosatellite attitude control. The multi-objective controller is designed based on linear model of attitude dynamics. The H_∞ performance takes into account both robustness stability against moments-of-inertia uncertainty and the disturbance rejection aspect. H₂ performance takes into account the LQG aspect which avoids the undesirable wheels’ saturation effect. In addition, the closed-loop poles can be forced into some sector of the stable half-plane to obtain well-damped transient responses. The problem is then reduced to a convex optimization involving linear matrix inequalities (LMIs), so it can be efficiently solved. The simulation results demonstrate that the presented mixed H₂/H_∞ control system is robust stable and optimal in the sense of H₂ norm, and has good steady-state and dynamic performances against the parameter uncertainties and various disturbances for the microsatellite attitude control system.     

某卫星挠性附件姿态动力学研究

根据导出的某有大型太阳帆板的挠性卫星数学模型,分析了模型中挠性振动对质心和姿态运动的影响,给出了卫星系统的动力学方程,并对帆板展开、卫星稳态运行的模型作工程化处理。分析和仿真结果表明：该方法能降低模型的复杂度,满足大型卫星的姿态指向精度和稳定度要求。     

Research Advances of Solar Corona and Interplanetary Physics in China: 2012–2014

Solar transients and their related interplanetary counterparts have severe effects on the space environments of the Earth. Therefore, the research of solar corona and interplanetary physics has become the focus of study for both solar and space scientists. Considerable progress has been achieved in these aspects by the solar and space physics community of China during 2012–2014, which will be given in this report. The brief report summarizes the research advances of solar corona and interplanetary physics into the following parts: solar wind origin and turbulence, coronal waves and seismology, solar eruptions, solar energetic particle and galactic cosmic ray, magnetic reconnection,Magnetohydrodynamic(MHD) models and their applications, waves and structures in solar wind,propagation of ICMEs/shocks and their arrival time predictions. These research achievements have been achieved by Chinese solar and space scientists independently or via international collaborations.     

Heat storage and electricity generation in the Moon during the lunar night

One of the biggest challenges of the exploration of the Moon is the survival of the crew and the lunar assets during the lunar night. The environmental conditions on the lunar surface and its cycle, with long periods of darkness, make any long mission in need of specific amounts of heat and electricity to be successful. We have analyzed two different systems to produce heat and electricity on the Moon's surface. The first system consists of Thermal Wadis, sources of thermal power that can be used to supply heat to protect the exploration systems from the extreme cold during periods of darkness. Previous results showed that Wadis can supply enough heat to keep lunar devices such as rovers above their minimum operating temperature (approximately 243 K). The second system studied here is the Thermal Energy Storage (TES), which is able to run a heat engine during the lunar night to produce electricity. When the Sun is shining on the Moon's surface, the system can run the engine directly using the solar power and simultaneously heat a thermal mass. This thermal mass is used as a high temperature source to run the heat engine during the night. We present analytical and numerical calculations for the determination of an appropriate thermal mass for the TES system.