环绕器次表层探测雷达实时处理技术

环绕器次表层探测雷达能够在环绕轨道实现行星次表层结构高分辨探测,为深入研究行星地质结构提供科学数据,由于深空探测距离地球距离非常遥远,与地球之间的数据传输率很受限制,雷达探测得到的大量原始数据无法通过数据链路传回地球,通过星上实时处理对探测数据进行变换,只回传数据量小得多的处理结果具有非常重要的意义。本文对环绕器次表层探测雷达采用的后向投影算法的实时处理技术进行了详细的分析,给出了工程实现方法。     

大行星、月球和小天体环绕型探测器的轨道问题

针对环绕型探测器的轨道,以具有不同物理特征的大天体(金星、火星和月球等)为例,根据它们的质量大小(决定其引力作用范围的大小)、密度分布和形状特征(决定其非球形引力场的特征),具体阐述了它们各自环绕型探测器轨道的可能形式和不同的变化特征,另外介绍了小天体探测时的两种伴飞形式。关于环绕型探测器的轨道特征,如月球无大气,对其低轨探测器而言没有能量耗散影响,却同样有轨道寿命问题,而且由于其质量分布不均匀,这种现象还与轨道倾角有密切关系;而对火星的环绕型探测器而言,尽管有类似现象,但与轨道倾角的关系却大不相同。这些重要的轨道变化特征,可为深空探测中目标轨道的选择和设计提供依据。     

改进的万有引力公式

根据广义相对论给出的行星运动方程，导出如下改进的万有引力公式F＝－GMm/r^2-3G^2M^2mp/c^2r^4应用该公式可给出光线近日偏折问题的准确解。     

行星轮系动态特性分析

针对某一具有五个行星轮的2K-H型行星齿轮传动系统,建立了多自由度系统的动力学模型,采用Gill法对系统的运动微分方程进行数值积分,得到了此多自由度系统在刚度激励作用下的动态响应,并计算了轮齿间的动态载荷,其中着重考虑了齿轮接触比和太阳轮中心浮动对动态特性的影响。      

宇宙真空测量的理论与技术

在行星上和在航天器上测量行星表面同一时刻、同一位置的大气密度,会得到不同的测量数据,必须经过坐标系转换把航天器上的测量数据转换成行星坐标系的数据才可和地面观测数据比较。文章系统地归纳了宇宙真空测量的理论与技术,改正了相应的坐标转换公式,对之进行了合理性讨论,推导出分子流密度和大气压强的转换公式并建立了地面校准宇航速度定向分子流压强及压强的模拟理论,形成了比较完整的宇宙真空测量理论体系。从该理论体系出发,提出了宇宙真空测量技术方案的建议。     

Cosmic background radiation from pregalactic objects

X-ray astronomy satellite TENMA observed that the X-ray pulsation of Vela X-1 suddenly disappeared for tens of minutes. This phenomenon may be interpreted in terms of the eclipse by a planet of HD77581, the optical companion of Vela X-1.     

An AO-free coronagraph experiment in vacuum with a binary-shaped pupil mask

We present our first results from laboratory experiments on a binary-shaped checkerboard mask coronagraph that was fitted inside a vacuum chamber for the development of skills to the direct observation of extra-solar planets. The aim of this work was to utilize a vacuum chamber for our coronagraph experiments in order to achieve an environment with higher thermal stability and which is free from air turbulence. We also aimed to evaluate and improve the performance of such a system consisting of a vacuum chamber with a coronagraph set inside the chamber. Both the raw contrast and the contrast after point spread function (PSF) subtraction are evaluated. We sited the vacuum chamber in a clean room, and we installed an optical fiber coupled to a visible He–Ne laser, appropriate coronagraph optics, a temperature sensor and heaters in the chamber. This provided a vacuum environment and a temperature-controlled environment with a visible light source, and was shown to improve the stability of the coronagraph. A contrast of 1.7×10^-7$1.7\times {10}^{-7}$ was achieved for the raw coronagraphic images by analyzing the areal mean of all of the observed dark regions. A contrast of 7.3×10^-9$7.3\times {10}^{-9}$ was achieved for the PSF subtraction by areal variance (1σ) of all of the observed dark regions. Speckles were a major limiting factor throughout the dark regions of both the raw images and the PSF subtracted images. The application of PSF subtraction for the Space Infrared telescope for Cosmology and Astrophysics (SPICA) and for other platforms is discussed.