汶川地震灾区影像地图的研制

结合汶川地震期间分县、1:25 000和1:5 000应急影像地图的设计与生产,对一些相关技术进行了试验和总结,可为今后影像地图的研制提供理论和方法上的参考.     

卫星遥感资料在山区洪涝灾害监测及决策服务中的应用

为充分发挥卫星遥感在防灾减灾工作中的应用,该文以2020年遵义市正安县汛期发生的特大暴雨洪涝灾害为研究个例,通过卫星搭载的合成孔径雷达的遥感影像反演,识别强降水影响区域,分级标识灾害风险,探索山区的三个叫应,以期发挥卫星遥感在防灾减灾中的作用,为防汛救灾和流域的上下游联防提供参考。结果表明：(1)山区防汛指挥调度,既要关注强降雨区域,也要考虑河流走向、上下游降水增叠效应,尤其是对于高大山脉前海拔高差明显区域的地表径流汇流增强作用,应加强判断联动叫应;(2)降雨量大小和地表水体增加量、存在的灾害风险隐患未必成正比,防汛工作不能一味只根据降雨量大小来做出灾害防范决定;(3)该案例作为一次天气过程造成影响的试点分析,为进一步探索对应关系提供参考基础,叫应关系的最终确立需要更多天气过程案例的统计分析。研究结果对正安县洪涝灾害防御决策指挥具有重要补充意义。     

GEOSAT卫星的ERM测高数据处理与中国近海海平面

对ＧＥＯＳＡＴ测高卫星在中国近海区域（０°－３５°Ｎ,１０５°－１２７°Ｅ）以及１２７°－１３５°Ｅ内６个ＥＲＭ周期（１９８７年１月１日－４月１２日）的地球物理数据记录（ＧＤＲ）中的数据进行了编辑和预处理．根据卫星弧段的实际长度选取了混合轨道误差模型,并采用最小二乘技术对上升弧段与下降弧段交叠点处的不符值进行了平差计算．处理结果表明,所选用的方法可以大大地消除径向轨道误差的影响,使交叠点处的不符值由原来的５６ｃｍ（ＲＭＳ）降低到现在的２４ｃｍ（ＲＭＳ）在此基础上,构造出６个１°×１°的中国近海海平面及其平均海平面．该平面被称为＂测高大地水准面＂与美国Ｏｈｉｏ州立大学的ＯＳＵ９１Ａ重力场模型的大地水准面相比,两者具有同等量级的精度及一致的形态。     

The dynamical environment of Dawn at Vesta

Dawn is the first NASA mission to operate in the vicinity of the two most massive asteroids in the main belt, Ceres and Vesta. This double-rendezvous mission is enabled by the use of low-thrust solar electric propulsion. Dawn will arrive at Vesta in 2011 and will operate in its vicinity for approximately one year. Vesta's mass and non-spherical shape, coupled with its rotational period, presents very interesting challenges to a spacecraft that depends principally upon low-thrust propulsion for trajectory-changing maneuvers. The details of Vesta's high-order gravitational terms will not be determined until after Dawn's arrival at Vesta, but it is clear that their effect on Dawn operations creates the most complex operational environment for a NASA mission to date. Gravitational perturbations give rise to oscillations in Dawn's orbital radius, and it is found that trapping of the spacecraft is possible near the 1:1 resonance between Dawn's orbital period and Vesta's rotational period, located approximately between 520 and 580 km orbital radius. This resonant trapping can be escaped by thrusting at the appropriate orbital phase. Having passed through the 1:1 resonance, gravitational perturbations ultimately limit the minimum radius for low-altitude operations to about 400 km, in order to safely prevent surface impact. The lowest practical orbit is desirable in order to maximize signal-to-noise and spatial resolution of the Gamma-Ray and Neutron Detector and to provide the highest spatial resolution observations by Dawn's Framing Camera and Visible InfraRed mapping spectrometer. Dawn dynamical behavior is modeled in the context of a wide range of Vesta gravity models. Many of these models are distinguishable during Dawn's High Altitude Mapping Orbit and the remainder are resolved during Dawn's Low Altitude Mapping Orbit, providing insight into Vesta's interior structure. Ultimately, the dynamics of Dawn at Vesta identifies issues to be explored in the planning of future EP missions operating in close proximity to larger asteroids.     

2011年7月24—25日呼伦贝尔市强降雨天气过程分析

利用常规气象资料、多普勒雷达资料和红外云图资料,对2011年7月24—25日呼伦贝尔市一次强降雨天气过程进行成因分析。结果表明：当鄂霍次克海阻塞高压强盛西伸并稳定少动,形成强大的阻挡系统时,使得西来低槽在我市西部停滞少动为强降水发生提供了有利的环流背景。中低层深厚的湿层以及西南低空急流为强降水提供充沛的水汽及能量条件。地面冷锋位置适宜且稳定少动为强降水提供了冷暖空气的触发条件。本地强对流天气潜势指数都充分表明层结的不稳定。卫星云图及雷达产品均有一定的指示意义。     

鄱阳湖水域面积与湖口水位关系模型的改进

利用2005年4月至2010年5月湖口水位资料和新一代极轨卫星（Terra）遥感的鄱阳湖水域面积资料,研究发现它们已经不满足原有鄱阳湖水域面积与湖口水位的关系模型（基于NOAA遥感资料）。运用最小二乘法和多项式拟合方法,综合考虑模拟与Terra卫星遥感的鄱阳湖水域面积的均方差和湖口极端水位下的拟合情况,发现在1—10次幂的多项式拟合中5次幂的多项式拟合效果最好,并根据5次幂的多项式拟合建立了鄱阳湖水域面积与湖口水位关系的新的关系模型。新的关系模型模拟性能较好,Terra卫星观测的与模拟的鄱阳湖水域面积的相关系数达到了0.982,且有95%的观测与模拟的偏差都小于200 km2。最后,利用2011年1—10月的Terra卫星观测资料和湖口水位资料,对新的关系模型的模拟性能进行了验证。     

卫星信标信道模拟器的设计与应用

针对卫星信标电离层测量系统研制及测试、验证的需要,设计卫星信标信道模拟器,阐述了卫星信标信道模拟器的技术指标、功能、原理和软、硬件实现方法;给出卫星信标信道模拟器的主要应用场合和应用方案。卫星信标信道模拟器的应用,将为卫星信标电离层测量系统的研制提供有利保障。     

基于资源三号卫星影像的1∶50000数据生产试验

我国自主研发的立体测绘卫星资源三号已经成功发射,并开始获取影像,应用前景广阔。本文通过利用资源三号卫星遥感影像试验生产1∶50 000 DLG,DEM,DOM等地理信息产品,分析其影像特点,详细探讨其在1∶50 000地理信息产品生产中的可行性、适用性和精度情况。     

Large-scale zonal flow and magnetic field generation due to drift-Alfven turbulence in ionosphere plasma

In the present work, the generation of large-scale zonal flows and magnetic field by short-scale collision-less electron skin depth order drift-Alfven turbulence in the ionosphere is investigated. The self-consistent system of two model nonlinear equations, describing the dynamics of wave structures with characteristic scales till to the skin value, is obtained. Evolution equations for the shear flows and the magnetic field is obtained by means of the averaging of model equations for the fast-high-frequency and small-scale fluctuations. It is shown that the large-scale disturbances of plasma motion and magnetic field are spontaneously generated by small-scale drift-Alfven wave turbulence through the nonlinear action of the stresses of Reynolds and Maxwell. Positive feedback in the system is achieved via modulation of the skin size drift-Alfven waves by the large-scale zonal flow and/or by the excited large-scale magnetic field. As a result, the propagation of small-scale wave packets in the ionospheric medium is accompanied by low-frequency, long-wave disturbances generated by parametric instability. Two regimes of this instability, resonance kinetic and hydrodynamic ones, are studied. The increments of the corresponding instabilities are also found. The conditions for the instability development and possibility of the generation of large-scale structures are determined. The nonlinear increment of this interaction substantially depends on the wave vector of Alfven pumping and on the characteristic scale of the generated zonal structures. This means that the instability pumps the energy of primarily small-scale Alfven waves into that of the large-scale zonal structures which is typical for an inverse turbulent cascade. The increment of energy pumping into the large-scale region noticeably depends also on the width of the pumping wave spectrum and with an increase of the width of the initial wave spectrum the instability can be suppressed. It is assumed that the investigated mechanism can refer directly to the generation of mean flow in the atmosphere of the rotating planets and the magnetized plasma.     

Long-term evolution of orbits about a precessing oblate planet. 2. The case of variable precession

We continue the study undertaken in Efroimsky [Celest. Mech. Dyn. Astron. 91, 75–108 (2005a)] where we explored the influence of spin-axis variations of an oblate planet on satellite orbits. Near-equatorial satellites had long been believed to keep up with the oblate primary’s equator in the cause of its spin-axis variations. As demonstrated by Efroimsky and Goldreich [Astron. Astrophys. 415, 1187–1199 (2004)], this opinion had stemmed from an inexact interpretation of a correct result by Goldreich [Astron. J. 70, 5–9 (1965)]. Although Goldreich [Astron. J. 70, 5–9 (1965)] mentioned that his result (preservation of the initial inclination, up to small oscillations about the moving equatorial plane) was obtained for non-osculating inclination, his admonition had been persistently ignored for forty years. It was explained in Efroimsky and Goldreich [Astron. Astrophys. 415, 1187–1199 (2004)] that the equator precession influences the osculating inclination of a satellite orbit already in the first order over the perturbation caused by a transition from an inertial to an equatorial coordinate system. It was later shown in Efroimsky [Celest. Mech. Dyn. Astron. 91, 75–108 (2005a)] that the secular part of the inclination is affected only in the second order. This fact, anticipated by Goldreich [Astron. J. 70, 5–9 (1965)], remains valid for a constant rate of the precession. It turns out that non-uniform variations of the planetary spin state generate changes in the osculating elements, that are linear in , where is the planetary equator’s total precession rate that includes the equinoctial precession, nutation, the Chandler wobble, and the polar wander. We work out a formalism which will help us to determine if these factors cause a drift of a satellite orbit away from the evolving planetary equator.By “precession,” in its most general sense, we mean any change of the direction of the spin axis of the planet—from its long-term variations down to nutations down to the Chandler wobble and polar wander.