低轨恒速平板型轨道分子屏与大气的撞击作用

以经典的气体分子运动论计算了低轨道（３００ｋｍ）恒速飞行的５ｍ直径平板型轨道分子屏所受的环境大气的撞击作用。大气分子和轨道分子屏的相互作用取完全弹性碰撞和完全非弹性碰撞这两种极端形式,由此可认为轨道分子屏所受的撞击作用就介于这两者之间。计算结果表明,六种主要的大气成分中,原子氧的撞击作用最大,约占总的撞击动量的８０％,Ａｒ的撞击作用最小,要比原子氧小４个数量级,作用于分子屏的总的作用力为０．０４１Ｎ～０．０８２Ｎ。这些数据将有助于更详尽的了解轨道分子屏在空间飞行时的行为。     

W33A的羟基分子脉泽辐射

本文给出了Ｗ３３Ａ在两个跃迁频率上的左右图偏振ＯＨ脉泽辐射谱线，采用细管和球模型，获得脉泽活动区的氢分子数密度近似１０７ｃｍ３．为了获得１０４６ｓ１量级脉泽光子发射率，两种模型一致要求抽运率为１（ＯＨ）ｃｍ３ｓ１，但球型脉泽活动区要求较高的抽运效率．     

小推力轨道优化研究

研究小推力电推进轨道优化问题,推力加速度量级为１０＾－２～１０＾－４,优化方法间接法,利用末端横截条件反向积分伴随方程,避开伴随变量的初值猜测,运用迭代法数值求解了逃兔地心引起场轨道和低轨道变轨优化,计算结果表明,小推力作用下最优转移轨道几乎为圆形,转移时间较长,小推力大小与作用时间成近似线反比关系,小推力情况下,横向比最优控制更为合理。     

星际分子的形成

广泛存在的星际分子１９６３年，由于射电望远镜的使用，人们开始陆续发现遥远的星际云中含有一些星际分子。此后，对星际分子的研究获得了很大的进展，星际分子也是２０世纪６０年代天文学上的四大发现之一。那个时候，天文学家谈论星际分子成了一种时髦。这些星际分子种类繁多，在空间的各个方向都发现了它们的踪迹，主要分布在银河系的旋臂中。在众多的星际分子云中，人们研究最多的是人马座B２和猎户座A，已发现的绝大多数分子在这里都可以找到。人马座B２被称为星际分子的宝库。现在，已发现的星际分子多达１００多种，主要有OH、H…     

微波电离型原子氧源的降能和中性化系统

在把微波电子回旋共振技术应用到离子源中,获得了１０＾１５个原子／（ｃｍ＾３．ｓ）束流的基础上,采用了结构新的降能和中性化系统,把高能氧离子转变为低能氧原子;成功地研制出了一种新颖的原子氧环境效应地面模拟试验装置。由该装置获得的粒子在能量和类型方面均与低地球轨道环境相一致,从而实现了对低地球轨道环境的真实模拟。     

利用卫星两行轨道根数反演热层密度

两行轨道根数（TLEs）是基于一般摄动理论产生的用于预报地球轨道飞行器位置和速度的一组轨道参数,通过求解大气阻力微分方程,可反演出热层大气密度. 本文选取近圆轨道CHAMP卫星和椭圆轨道Explorer8卫星,以两行轨道根数数据为基础,计算反弹道系数,并根据不同轨道特征采用两种不同反演方法对热层大气密度进行研究. 结果表明,这两种方法反演得到的大气密度与实测值均符合较好,其中CHAMP卫星的反演结果和经验模式值相对于实测值的误差分别为7.94%和13.94%,Explorer8卫星的误差分别为9.04%和14.32%. 相比模式值,利用两行轨道根数数据反演的热层大气密度更接近于实测值,说明该方法可以作为获取大量可靠大气密度数据的一种有效途径.      

轨道误差对星敏感器对地指向精度的影响分析

针对使用星敏感器进行对地指向精度问题,分析了影响卫星对地指向精度的主要因素,根据卫星轨道误差,推导了轨道根数误差对经度方向和纬度方向上的指向误差方程.分析了轨道根数对指向精度的影响规律.最后对轨道根数误差的影响进行了仿真,仿真结果与分析结果一致.     

代谢起源进化的分子模拟研究

新陈代谢为生命提供了物质和能量基础，与生命起源和进化密切相关.然而，由于缺乏化石证据，代谢的起源及其影响生物进化的分子机制等重要问题尚待解决.近年来，网络扩张算法等分子模拟方法的出现为解决这些问题提供了新途径.本文综述了近年来代谢起源进化的分子模拟研究，以期为相关领域学科发展提供新思路.      

大气密度变化对卫星返回轨道参数的影响

本文在考虑大气密度(90km高度以下) 随地理纬度、高度及时间(月份)随机变化的基础上,沿卫星的返回轨道建立了随机大气密度的统计模型。并应用该模型产生的随机大气密度样本,进行返回轨道的Monte Corlo法模拟计算。通过对模拟计算得到的返回轨道参数样本的统计处理,本文分析了大气密度变化对卫星返回轨道参数的影响。另外,本文还介绍了近似估计大气密度变化对返回轨道参数影响的影响系数法。     

“菲莱”探测到有机分子

据报道，欧空局的彗星登陆器“菲莱”在主电池耗尽之前，已经探测到了有机分子。含碳有机分子是地球生命的基础，这一发现有助于我们了解地球生命的起源。     

高速RS编码器的FPGA实现

ＲＳ码广泛应用于卫星通信,移动通信和数据存储等领域中,研究用现场可编程编辑阵列（ＦＰＧＡ）实现高速ＲＳ码编码器;对硬件实现中的主要问题做了分析和讨论,仿真和实际测试结果均表明,编码器原理样机功能正常,吞吐率可达２００Ｍｂｉｔ／ｓ。     

微重力场中通风换热的数值研究

为在地面模拟空间站舱内的流动与换热,以两顶角集中进风,两底角集中出风的通风方式为对象,研究了微重力是条件下复杂深间内的对流换热地面相似模拟问题,采用数值分析方法,分别考察了方腔中无隔离物,有绝热隔离物,有等温隔离物以及有等温悬浮物的几种有代表性的不同情形,给出了每种情形下不同比例模型的流动与换热情况的数值模拟结果,并针对各种不同情形进行了分析说明,分析表明,集中通风方式更有利于抑制自然对流的影响。     

空间站伴随卫星的轨道及形成分析

空间站伴随卫星是在空间站附近周期运动、为空间站提供特殊服务的航天器。论述了空间站伴随卫星的概念;分析了空间站伴随卫星的轨道及形成; 给出了空间站伴随卫星理想伴随轨道形成的条件。     

烧蚀材料光谱发射率测量及高温总发射率计算

采用辐射能量法测量了三种烧蚀材料的中温光谱发射率，提出了由所测中温光谱发射率计算烧蚀材料的高温发射率的方法，此外，还推导了由不同波段的发射率计算材料总发射率的公式。     

Radio occultation electron density profiles from the FORMOSAT-3/COSMIC satellites over the Brazilian region: A comparison with Digisonde data

This study aims to validate the electron density profiles from the FORMOSAT-3/COSMIC satellites with data from Digisondes in Brazil during the low solar activity period of the years 2006, 2007 and 2008. Data from three Brazilian Digisondes located in Cachoeira Paulista (22.7°S, 45°W), São Luís (2.5°S, 44.2°W) and Fortaleza (3.8°S, 38°W) were used in the comparisons. Only the profiles whose density peak have been obtained near the stations coordinates were chosen for the comparison. Although there is generally good agreement, some cases of discrepancies are observed. Some of these discrepancies cannot be explained simply by the differences in the position and local time of the measurements made by the satellite and the ground-based station. In such cases it is possible that local conditions, such as the presence of a trans-equatorial wind or electron density gradients, could contribute to the observed differences. Comparison of the F2 layer peak parameters, the NmF2 and hmF2, obtained from the two techniques showed that, in general, the agreement for NmF2 is pretty good and the NmF2 has a better correlation than hmF2. Cachoeira Paulista had the worst correlation for hmF2 possibly because this station is situated in the region under the influence of the equatorial ionization anomaly, a region where it is more difficult to apply the RO technique without violating the spherical symmetry condition.     

声重波激发的赤道 Spread—F 不稳定性

本文导出了声重波扰动与赤道电离层扩展F层相互作用的基本方程,并对数值模拟结果进行了讨论。结果表明当声重波扰动与Kavleigh-Taylor不稳定性共同作用于赤道F层时,将导致大尺度波状结构的Spread-F.其特征为以一定速度漂移的准周期不规则性,发展到后期伴有羽柱形状的bubble(电子密度低区)产生。这种现状的bubble可上升至F层顶部并发生倾斜。声重波波矢量的方向决定着羽柱的倾斜方向。这些结果与实验观测特征相符,说明声重波扰动不仅是大尺度Saread-F的触发源,而且对其整个形态发展过程起着重要的作用。      

Observation of the north-south asymmetry in the equatorial spread F intensity at the Brazilian longitude

This study presents an analysis of the observed north-south asymmetry of the range spread F (RSF) intensity at the low latitude region during an equinoctial month of different solar epochs (2002, 2015 and 2017). The ionospheric parameters were obtained during geomagnetic quiet days from four digisonde stations located along the Brazilian longitude, which include a dip equator station (Sao Luiz (SL: 2.33 S, 44.2 W)), conjugate stations (Campo Grande (CG: 20.5°S, 55°W) and Boa Vista (BV: 2.8°N, 60.7°W)) and another low latitude station (Cachoeira Paulista (CP: 22.7°S, 45°W)). The results highlight the competing effect of the post-sunset electric field strength and the trans-equatorial wind on the latitudinal distribution of the irregularity intensity at both hemispheres under varying background ionospheric condition. The RSF intensity was seen to reduce as the solar flux index decreased and the latitudinal peak shifted closer to the dip equator. This was dependent on the variation of the field line mapped irregularity spectrum and the density gradient. Likewise, the north-south asymmetry in the irregularity occurrence was seen to become more significant as a denser ionosphere was observed at the hemisphere with the equatorward meridional wind. This has further proven that the non-linear cascading of the plasma irregularity across the low latitude region is strongly influenced by the local electric field.     

RAMAN SPECTRA OF SEVEN INTERPLANETARY DUST PARTICLES

The Raman Shift Spectra of seven interplanetary dust particles,U2034 (F10),U2034(F8),U2022(B1),W7074 18,W7074 C15,W7074 C3 and W7074 A7,were measured with a Spex-1403 Raman Spectrograph.The exciting radiations were the 488 nm and 514 nm line of a 5W argon ion laser.All seven spectra exhibit the 1350 and 1600 Acm-1 arbon bands,implying that the IDPS were coated with hydrocarbon and incompletely crystallized carbon,the part of which may be the residue of hydro-carbon contents in the particles after water loss by the heating during their entry into the earth's atmosphere.A weak band structure in the 520-610 cm-1 range could be caused by cyclosilicates,and a weak band at 2900 cm-1 is tentatively identified as due to hydrocarbon molicules.     

Possible physical properties of the flow in the vicinity of the heliopause

An interface between the fully ionized hydrogen plasma of the solar wind (SW) and the partially ionized hydrogen gas flow of the local interstellar medium (LISM) is formed as a region where there is a strong interaction between these two flows. The interface is bounded by the solar wind termination shock (TS) and the LISM bow shock (BS) and is separated on two regions by the heliopause (HP) separating the solar wind and charged component of the LISM (plasma component below). The BS is formed due to the deceleration of the supersonic LISM flow relative to the solar system. Regions of the interface between the TS and HP and between the HP and BS were in literature named as the inner and outer heliosheaths, respectively. An investigation of the structure and physical properties of the heliosheath is at present especially interested due to the fact that Voyager-1 and Voyager-2 have crossed the TS in December 2004 (Burlaga, L.F., Ness, N.F., Acuna, M.Y., et al. Crossing the termination shock into the the heliosheath. Magnetic fields. Science 309, 2027–2029, 2005; Fisk, L.A. Journey into the unknown beyond. Science 309, 2016–2017, 2005; Decker, R.B., Krimigis, S.M., Roelof, E.C., et al. Voyager 1 in the foreshock, termination shock and heliosheath. Science 309, 2020–2024, 2005; Stone, E.C., Cummings, A.C., McDonald, F.B., et al. Voyager 1 explores the termination shock region and the heliosheath beyond. Science 309, 2017–2020, 2005) and in September 2007 (Jokipii, J.R. A shock for Voyager 2. Nature 454, 38–39, 2008; Gurnett, D.A., Kurth, W.S. Intense plasma waves at and near the solar wind termination shock. Nature 454, 78–80, 2008. doi: 10.1038/nature07023; Wang, L., Lin, R.P., Larson, D.E., Luhmann, J.G. Domination of heliosheath pressure by shock-accelerated pickup ions from observations of neutral atoms. Nature 454, 81–83, 2008. doi: 10.1038/nature07068.14; Burlaga, L.F., Ness, N.F., Acuna, M.H., et al. Magnetic fields at the solar wind termination shock. Nature 454, 75–77, 2008. doi: 10.1038/nature07029; Richardson, J.D., Kasper, J.C., Wang, C., et al. Cool heliosheath plasma and deceleration of the upstream solar wind at the termination shock. Nature 454, 63–66, 2008. doi: 10.1038/nature07024; Stone, E.C., Cummings, A.C., McDonald, F.B., et al. An asymmetric solar wind termination shock. Nature 454, 71–74, 2008. doi: 10.1038/nature07022; Decker, R.B., Krimigis, S.M., Roelof, E.C., et al. Mediation of the solar wind termination shock by non-thermal ions. Nature 454, 67–70, 2008. doi: 10.1038/nature 07030), respectively, and entered to the inner heliosheath.     

Effect of the seed perturbation amplitude on the equatorial spread F initiation during solar minimum

The contribution of gravity wave (GW) to the initiation/development of spread F during a solar minimum year was investigated through the comparison of the observed precursory parameters and characteristics of the corresponding equatorial spread F (ESF) events. The ionospheric parameters were recorded at the magnetic equatorial station Sao Luis (2.3°S, 44°W, dip latitude 2°S) during March and October 2010. These data were used to estimate the influence of the relative gravity wave amplitude and the ambient ionospheric condition on the diurnal variation of the spread F initiation. The vertical velocity drift indicated a clear control and defines the threshold for the seasonal variability of the ESF occurrence. However, it was insufficient to solely determine or predict the day to day variation of ESF occurrence. Thus, few days with contrasting ambient ionospheric condition and magnitude of GW amplitude were analysed in order to investigate the role of the different precursory factors in the observed diurnal variation of the plasma irregularity development. The density scale length and gravity wave amplitude were shown to immensely contribute to the linear instability growth rate, especially during the days with a low post-sunset rise. Thus, the experimental observations have demonstrated the strong inter-dependence between the precursory factors and they have also highlighted the probable control of the ESF morphology.