装备维修质量管理研究

分析了装备维修质量的基本内涵及其主要影响因素,就人为因素对装备维修质量的影响进行了重点分析,在此基础上有针对性地阐述了提出了相应的质量管理对策,加强培训、监督和建立迅捷维修信息管理系统等加强的质量管理的手段。     

利用区间广义卡尔曼滤波器跟踪来袭弹道式导弹

用雷达跟踪来袭弹道式导弹,由于其运动模型、测量噪声的不确定性,成为需要研究的重要问题。经典广义卡尔曼滤波器(EKF)不再适用于这种不确定的问题,因此,引入一种新的区间广义卡尔曼德波(EIKF)方法来跟踪导弹系统。计算机仿真结果表明本EIKF算法对于这种不确定的、非线性弹道式导弹的测量问题是有效的。     

南宁社会称谓语使用情况的调查分析

南宁市社会称谓语与职业、年龄等要素密切相关.文章以它们为考察切入点,分析了其社会称谓语的选择比例情况.     

交流伺服系统位置跟踪误差

首先提出采用比例和位置前馈复合控制的位置闭环调节器。位置前馈工作在完全补偿状态时,实现了恒速运行时间段内和定位结束后的稳态位置跟踪零误差。但由于目前广泛使用的梯形给定存在加速度突变,增大了动态位置跟踪误差,所以提出采用S曲线位置给定,避免加速度突变,可以大大减小动态位置跟踪误差。最后分析了负载变动对位置跟踪误差的影响,并提出了消除这种影响的途径和方法。仿真分析和实验结果证明了理论分析的正确性。     

Space-to-space Radio Interferometry System from Medium Earth Orbits

This paper presents a new concept to perform space-to-space Very Long Baseline Interferometry which enables the imaging of cosmic sources at high-resolution and high-sensitivity with small antennas. Several individual apertures are embarked on separate identical satellites staggered in height into Polar or Equatorial Circular Medium Earth Orbits (PECMEO orbits). These orbits are stable and allow GNSS-based on-the-fly centimeter-level relative positioning. Coherent operation is possible by exchanging local oscillator components and measured signals through Inter-Satellite Links (ISL). On-board cross correlation is performed at each satellite over a delay window compatible with the accuracy of the on-the-fly relative positioning and the result sent to the ground. Image reconstruction is completed on the ground thanks to sub-millimeter baseline retrieval from accurate GNSS orbits, ISL ranging and spacecraft attitude information. The application of this concept to image the Super Massive Black Hole Sgr A* is hinted.      

剪切同轴式喷嘴中心管壁厚对火焰的影响

为了研究剪切同轴式喷嘴中心管壁厚度对火焰的影响,针对LOX/CH4火焰,采用数值方法计算了三种不同喷嘴中心管壁厚的长方体形燃烧室内的燃烧过程,计算表明,对于较大的管壁厚度,在紧贴管壁下游的区域将形成较大的回流区,有利于火焰稳定在喷嘴出口处,还给出了采用相同几何结构燃烧室的LOX/CH4燃烧试验结果,试验也得出了同样的趋势,随着中心管壁厚度的增加,火焰中心明显前移。     

Coronal mass ejection (CME) activity of low mass M stars as an important factor for the habitability of terrestrial exoplanets. I. CME impact on expected magnetospheres of Earth-like exoplanets in close-in habitable zones

Low mass M- and K-type stars are much more numerous in the solar neighborhood than solar-like G-type stars. Therefore, some of them may appear as interesting candidates for the target star lists of terrestrial exoplanet (i.e., planets with mass, radius, and internal parameters identical to Earth) search programs like Darwin (ESA) or the Terrestrial Planet Finder Coronagraph/Inferometer (NASA). The higher level of stellar activity of low mass M stars, as compared to solar-like G stars, as well as the closer orbital distances of their habitable zones (HZs), means that terrestrial-type exoplanets within HZs of these stars are more influenced by stellar activity than one would expect for a planet in an HZ of a solar-like star. Here we examine the influences of stellar coronal mass ejection (CME) activity on planetary environments and the role CMEs may play in the definition of habitability criterion for the terrestrial type exoplanets near M stars. We pay attention to the fact that exoplanets within HZs that are in close proximity to low mass M stars may become tidally locked, which, in turn, can result in relatively weak intrinsic planetary magnetic moments. Taking into account existing observational data and models that involve the Sun and related hypothetical parameters of extrasolar CMEs (density, velocity, size, and occurrence rate), we show that Earth-like exoplanets within close-in HZs should experience a continuous CME exposure over long periods of time. This fact, together with small magnetic moments of tidally locked exoplanets, may result in little or no magnetospheric protection of planetary atmospheres from a dense flow of CME plasma. Magnetospheric standoff distances of weakly magnetized Earth-like exoplanets at orbital distances 相似文献   

Porphyrin as an ideal biomarker in the search for extraterrestrial life

A key issue in astrobiological research is identifying target molecules that are unambiguously biological in origin and can be easily detected and recognized. We suggest porphyrin derivatives as an ideal target, because these chromophores are global in distribution and found in virtually all living organisms on Earth, including microorganisms that may approximate the early evolution of life on Earth. We discuss the inherent qualities that make porphyrin ideally suited for astrobiological research and discuss methods for detecting porphyrin molecules in terrestrial sedimentary environments. We present preliminary data to support the use of ToFSIMS as a powerful technique in the identification of porphyrins.     

Role of the ionosphere for the atmospheric evolution of planets

We have synthesized current understanding, mainly observations, with regard to ion escape mechanisms to space from the ionosphere and exosphere of Titan and Earth-type planets, with the intent to provide an improved input for models of atmospheric evolution on early Earth and Earth-type planets and exoplanets. We focus on the role of the ionosphere and its non-linear response to solar parameters, all of which have been underestimated in current models of ancient atmospheric escape (4 billion years ago). Factors that have been overlooked include the following: (1) Much larger variation of O(+) outflow than H(+) outflow from the terrestrial ionosphere, depending on solar and geomagnetic activities (an important consideration when attempting to determine the oxidized state of the atmosphere of early Earth); (2) magnetization of the ionopause, which keeps ionospheric ions from escaping and controls many other escape processes; (3) extra ionization by, for example, the critical ionization velocity mechanism, which expands the ionosphere to greater altitudes than current models predict; and (4) the large escape of cold ions from the dense, expanded ionosphere of Titan. Here we offer, as a guideline for quantitative simulations, a qualitative diagnosis of increases or decreases of non-thermal escape related to the ionosphere for magnetized and unmagnetized planets in response to changes in solar parameters (i.e., solar EUV/FUV flux, solar wind dynamic pressure, and interplanetary magnetic field).