木星和土星冰卫星上的撞击坑分布:探寻外太阳系撞击体来源的钥匙

充分认识外太阳系撞击体的来源类型和分布特征,对认识外太阳系固态天体上撞击过程,明确外太阳系天体上的撞击坑生成率和撞击坑定年等诸多方面具有重要的意义.得益于海量高质量探测数据的获取,如今我们对内太阳系主要天体表面的撞击分布和来源已经有了较为深入的了解,但对外太阳系天体的撞击分布和来源还知之甚少.不同大小频率的撞击体会在外太阳系冰卫星表面形成不同大小频率分布的撞击坑,不同飞行速度的撞击体也会在同步自转的冰卫星上留下程度不同的前导-后随半球不对称分布的撞击坑,因此,对外太阳系冰卫星上撞击坑的大小频率分布和前导-后随半球不对称性分布的观测,可以用于反推外太阳系的主要撞击来源.木星系统中大坑(D＞10～30 km)的主要撞击来源是日心小天体(环绕太阳),但目前在木卫三和木卫四上观测到的前导-后随半球不对称性程度与黄道彗星引起的不对称性程度并不相符,更接近于近各向同性彗星(NICs)引起的不对称性,这与目前的天文观测和理论计算结果不一致;木卫二上的大坑稀少,小坑(D＜1 km)则主要受一次坑的溅射物影响.对土星系统,土卫五和土卫八的大坑(D＞20～30 km)分布更符合日心小天体来源;而土卫一、土卫四、土卫三上的分布则与行心碎屑物(以行星为中心)一致,尤其是小坑更可能来自以土星为中心的撞击体影响,例如大型盆地的溅射物或卫星碎片残骸.     

飞机草总黄酮体外抑菌活性与体内抗大肠埃希菌感染效果

提取飞机草(Eupatorium odoratum Linn.)总黄酮,从抑菌圈、最小抑菌浓度(MIC)及最小杀菌浓度(MBC)等方面探讨飞机草总黄酮对金黄色葡萄球菌(Staphylococcus aureus)、鸡白痢沙门氏菌(Salmonella pullorum)、枯草芽孢杆菌(Bacillus subtilis)、大肠埃希菌(Escherichia coli)的体外抑菌活性;经腹腔注射大肠埃希菌感染小鼠后,灌胃给予飞机草总黄酮,观察供试小鼠腹泻率,测定小鼠粪便大肠埃希菌数及血清抗体水平(IgM、IgA和IgG),评价飞机草总黄酮的体内抗感染作用。结果表明,金黄色葡萄球菌对飞机草总黄酮最为敏感,其抑菌圈直径为19.50 mm,MIC为0.015 6 g/m L,MBC为0.031 3 g/m L;160 mg/kg的飞机草总黄酮可降低小鼠腹泻率和粪便大肠埃希菌数(P0.01),提高血清IgA(P0.01)和IgG含量(P0.05)。飞机草总黄酮具有体内、体外抗菌作用。     

遥感卫星在轨机场变化检测方法

针对机场飞机变化检测时效性要求高的特点,提出了遥感图像在轨变化检测的方法。该方法利用遥感卫星前后两幅机场图像,通过SURF方法配准并进行仿射变换,然后利用显著目标检测方法缩小目标检测区域,最后利用本文提出的圆周信息匹配方法,将二维图像匹配转换为一维信息检测的问题,实现对飞机的检测。利用前后两轨卫星遥感图像进行了试验,仿真结果表明,配准精度达到1个像素,能准确检测出飞机目标,说明该方法能准确高效地检测出机场飞机变化信息。     

基于ArcGIS Engine的飞机人工增雨航线自动化设计算法研究

人工增雨作为应急抗旱和缓解水资源紧张的重要手段,与社会经济可持续发展、生态安全和人民生活密切相关。航线设计是飞机人工增雨作业方案设计的一项重要内容,基于GIS平台自动化设计飞行航线将成为趋势。在传统飞行航线设计方案的基础上,研究提出了基于ArcGIS Engine的半圆弧过渡条播航线、＂弓＂字形条播航线和＂之＂字形条播航线三种层状云作业＂穿云＂航线与一种对流云或层积混合云作业＂绕云＂航线的自动化设计算法。应用结果显示,四种自动化算法均能够快速有效地设计出飞机航线,取得很好的效果。     

NASA电子眼让飞行员“看穿”雾霭

美国航空航天局(NASA)研制出的一款新型电子眼镜将被飞行员运用,帮助他们在雾天时安全驾驶飞机。这款电子眼镜是靠分布在驾驶舱四周的监视器和一个内置回转仪工作的,能制定出飞行员前方的透视图,对于飞行员在雾天     

A modified stratified model for the 3C 273 jet

We present a modified stratified jet model to interpret the observed spectral energy distributions of knots in the 3C 273 jet. Based on the hypothesis of the single index of the particle energy spectrum at injection and identical emission processes among all the knots, the observed difference of spectral shape among different 3C 273 knots can be understood as a manifestation of the deviation of the equivalent Doppler factor of stratified emission regions in an individual knot from a characteristic one. The summed spectral energy distributions of all ten knots in the 3C 273 jet can be well fitted by two components: a low-energy component (radio to optical) dominated by synchrotron radiation and a high-energy component (UV, X-ray and γ-ray) dominated by inverse Compton scattering of the cosmic microwave background. This gives a consistent spectral index of α= 0.88 (Sv α v-α) and a characteristic Doppler factor of 7.4. Assuming the average of the summed spectrum as the characteristic spectrum of each knot in the 3C 273 jet, we further get a distribution of Doppler factors. We discuss the possible implications of these results for the physical properties in the 3C 273 jet. Future GeV observations with GLASTcould separate the γ-ray emission of 3C 273 from the large scale jet and the small scale jet (i.e.the core) through measuring the GeV spectrum.     

Magnetic interactions during sympathetic solar eruptions

We present the first evidence for occurrences of magnetic interactions between a jet, a filament and coronal loops during a complex event, in which two flares sequen-tially occurred at different positions of the same active region and were closely associated with two successive coronal mass ejections (CMEs), respectively. The coronal loops were located outside but nearby the filament channel before the flares. The jet, originating from the first flare during its rise phase, not only hit the filament body but also met one of the ends of the loops. The filament then underwent an inclined eruption followed by the second flare and met the same loop end once more. Both the jet and the filament erup- tion were accompanied by the development of loop disturbances and the appearances of brightenings around the meeting site. In particular, the erupting filament showed clear manifestations of interactions with the loops. After a short holdup, only its portion passed through this site, while the other portion remained at the same place. Following the fila-ment eruption and the loop disappearance, four dimmings were formed and located near their four ends. This is a situation that we define as "quadrupolar dimmings." It appears that the two flares consisted of a sympathetic pair physically linked by the interaction between the jet and the filament, and their sympathy indicated that of the two CMEs.Moreover, it is very likely that the two sympathetic CMEs were simultaneously associ-ated with the disappearing loops and the quadrupole dimmings.     

飞机人工增雨作业效果分析

采用2009年12月～2010年1月广西飞机人工增雨作业数据,结合作业期间的相关气象资料,分析飞机人工增雨作业效果。结果表明,在影响广西的天气系统总体偏弱的情况下,实施飞机人工增雨作业后,雷达回波强度出现明显增强,降雨明显增加,降雨实况均比常年同期偏多,偏多程度在1成～2倍以上。     

河南春季一次层状冷云的微物理结构特征分析

利用2007年3月3日PMS粒子测量系统对河南层状云的探测资料,分析了云的微物理结构特征。结果表明,云垂直和水平分布不均匀特性很明显。在云的中上部,FSSP-100测量的小云粒子(云滴、冰晶)最大浓度为125个·cm~(-1),平均值为21.3个·cm~(-1),平均直径多在6～20μm。2D-C观测大云粒子(50d≤300μm)随高度上升浓度增多,浓度值变化在5.24～192个·L~(-1),平均直径为211μm。此层云中过冷液态水含量变化在0.035～0.118 g·m~(-3),随高度增加过冷液态水含量减少。在云的底部区域,观测到两个逆温层顶的下方分别存在有云水含量的峰值。由不同高度云粒子谱分析表明,在4046～4600 m高度层,粒子谱型有负指数型、单峰型、双峰型和多峰型;0℃层以下融化带内的粒子谱型多为负指数型;云的底部粒子谱型以负指数型和单峰型为主。