Expectations for Crater Size and Photometric Evolution from the Deep Impact Collision

The NASA Discovery Deep Impact mission involves a unique experiment designed to excavate pristine materials from below the surface of comet. In July 2005, the Deep Impact (DI) spacecraft, will release a 360 kg probe that will collide with comet 9P/Tempel 1. This collision will excavate pristine materials from depth and produce a crater whose size and appearance will provide fundamental insights into the nature and physical properties of the upper 20 to 40 m. Laboratory impact experiments performed at the NASA Ames Vertical Gun Range at NASA Ames Research Center were designed to assess the range of possible outcomes for a wide range of target types and impact angles. Although all experiments were performed under terrestrial gravity, key scaling relations and processes allow first-order extrapolations to Tempel 1. If gravity-scaling relations apply (weakly bonded particulate near-surface), the DI impact could create a crater 70 m to 140 m in diameter, depending on the scaling relation applied. Smaller than expected craters can be attributed either to the effect of strength limiting crater growth or to collapse of an unstable (deep) transient crater as a result of very high porosity and compressibility. Larger then expected craters could indicate unusually low density (< 0.3 g cm⁻³) or backpressures from expanding vapor. Consequently, final crater size or depth may not uniquely establish the physical nature of the upper 20 m of the comet. But the observed ejecta curtain angles and crater morphology will help resolve this ambiguity. Moreover, the intensity and decay of the impact “flash” as observed from Earth, space probes, or the accompanying DI flyby instruments should provide critical data that will further resolve ambiguities.     

TYC-1涂层材料热防护性能预测

根据TYC－1涂层材料在加热过程中所出现的物理化学变化，提出了三层物理模型，建立了相应的守恒方程和边界条件，并给出具有空间和时间二阶精度的差分离散公式，并按稳态和轨道模拟二类试验工况，预测了TYC－1防热涂层的内部温度分布，且与测量结果符合很好。     

江苏省CBERS-1卫星红外数据应用示范研究评价

文章对CBERS -1卫星IRMSS数据从空间分辨率、几何精度、噪声等方面作了分析评价 ,选取典型的南京地区、洪泽湖作为示范应用区 ,经过几何精纠正后的IRMSS数据进行不同地物在不同波段上的光谱采样分析 ,进行了城市信息与湖泊信息提取实验 ,效果较好 ,对南京辖区和洪泽湖的形态特征、环境因素、动态变迁等方面作了分析研究 ,从图像上可以清晰地看出南京辖区水体、城建和交通以及郊区的农林状况、洪泽湖河口淤积、岸边污染的情况。总之 ,CBERS-1卫星IRMSS数据可用 ,质量较好 ,达到了设计要求 ,有广阔的应用前景。     

遥感小卫星简介——以"北京一号"小卫星为例

高性能对地观测小卫星DMC 4--“北京一号”2005年10月27日在俄罗斯普列谢茨克发射场由宇宙3M火箭成功发射。文章针对小卫星的结构特点和数据特点,指出DMC小卫星图像数据具有获取灵活、重返周期短和大区域覆盖等优势,在地质灾害的调查、监测和预警工作中具有巨大的应用潜力。     

北京一号小卫星及其数据应用

结合小卫星技术介绍了北京一号高性能对地观测小卫星计划和项目进展情况,综述了北京一号系统的主要组成和性能,并结合其数据特点,介绍北京一号遥感影像的示范应用和重点应用,探讨、分析了其更广泛的应用领域和良好的市场前景。     

FY-1C/D极轨气象卫星空间粒子成分监测器及其在轨探测结果

介绍了风云一号(FY-1)C，D极轨气象卫星空间粒子成分监测器的任务目标、主要功能和工程指标。以及数据的获取和处理方法。给出了空间环境宁静期、地磁扰动事件、太阳质子事件、与太阳活动的关系和粒子长期变化等探测结果，并进行了相应的分析。对C，D星空间粒子成分监测器分别进行的5年和第二次在轨测试结果表明，两星监测器工作正常、性能稳定，探测数据可靠。     

GMSK信号的非相干解调技术研究

介绍了GMSK信号的两种非相干解调--1bit差分解调和改进型的Viterbi算法解调.通过计算机仿真对这两种非相干解调算法进行了研究,最后在相互之间进行了解调性能仿真比较.仿真结果表明,1bit差分解调算法完全能够实现对GMSK信号的正确解调, 改进型的Viterbi解调算法在解调过程中用MSK信号的相位路径进行高斯滤波后作为参考路径,并选取与接收信号的相位路径的Euclidean距离最小的作为解调路径,取得了良好的解调效果.在同等误码率要求下,改进的Viterbi算法比1bit差分解调性能具有更高的SNR优势.     

CBERS-1红外遥感器图像处理系统设计

红外多光谱扫描仪（IRMSS）是中巴地球资源卫星（CBERS）上的重要有效载荷之一。其获取的红外图像可以在国民经济的各个领域得到广泛应用。但是由数传系统传回的图像数据不能直接用,必须经过相应的处理。文章介绍的内容就是如何设计一个处理系统,将这种不可直接用数据经过解码和图像格式的处理,得到可视图像;经过图像预处理,得到零级图像;经过相应的辐射校正处理,得到一级图像:经过几何校正处理,得到二级图像产品,提供给其它经济各部门加以应用。     

Gas permeability and flow characterization of simulated lunar regolith

Recent discoveries of water ice trapped within lunar topsoil (regolith) have placed a new emphasis on the recovery and utilization of water for future space exploration. Upon heating the lunar ice to sublimation, the resulting water vapor could theoretically transmit through the lunar regolith, to be captured on the surface. As the permeability of lunar regolith is essential to this process, this paper seeks to experimentally determine the permeability and flow characteristics of various gas species through simulated lunar regolith (SLR). Two different types of SLR were compacted and placed into the permeability setup to measure the flow-rate of transmitted gas through the sample. Darcy’s permeability constant was calculated for each sample and gas combination, and flow characteristics were determined from the results. The results show that Darcy’s permeability constant varies with SLR compaction density, and identified no major difference in permeable flow between the several tested gas species. Between the two tested SLR types, JSC-1A was shown to be more permeable than NU-LHT under similar conditions. In addition, a transition zone was identified in the flow when the gas pressure differential across the sample was less than ∼40 kPa.     

Neuroimmune response and sleep studies after whole body irradiation with high-LET particles

In order to investigate the biological effects of galactic rays on astronaut cerebral functions after space flight, mice were exposed to different heavy ions (HZE) in whole-body conditions at doses comparable to the galactic flux: ¹²C, ¹⁶O and ²⁰Ne (95 MeV/u, at 42–76 mGy). Animals were also exposed to 42 mGy of ⁶⁰Co radiation for comparison with HZE. The neuroimmune response, evaluated by interleukin-1 (IL-1) measurement, showed that this cytokine was produced 3 h after irradiation by ¹⁶O or ⁶⁰Co. In contrast, neither ¹²C (56.7 mGy) nor ²⁰Ne (76 mGy) induced IL-1 production. However, immunohistochemical staining of ¹²C-irradiated mouse brain tissue showed 2 months later a marked inflammatory reaction in the hippocampus and a diffuse response in parenchyma. Sleep studies were realized before and after exposure to 42 mGy of ¹⁶O and 76 mGy of ²⁰Ne: only the ²⁰Ne radiation displayed a small effect. A slight decrease in paradoxical sleep, corresponding to a reduction in the number of episodes of paradoxical sleep, was manifested between 8 and 22 days after exposure. Exposure to ¹²C and ¹⁶O induced no changes either in cellularity of spleen or thymus, or in caspase 3 activity (as much as four months after irradiation). Taken together, these data indicate that the CNS could be sensitive to heavy ions and that responses to HZE impact depend on the nature of the particle, the dose threshold and the time delay to develop biological processes. Differences in responses to different HZE highlight the complex biological phenomena to which astronauts are submitted during space flight.