Observations of Vertical Reflections from the Topside Martian Ionosphere

The Martian ionosphere has for the first time been probed by a low frequency topside radio wave sounder experiment (MARSIS) (Gurnett et al., 2005). The density profiles in the Martian ionosphere have for the first time been observed for solar zenith angles less than 48 degrees. The sounder spectrograms typically have a single trace of echoes, which are controlled by reflections from the ionosphere in the direction of nadir. With the local density at the spacecraft derived from the sounder measurements and using the lamination technique the spectrograms are inverted to electron density profiles. The measurements yield electron density profiles from the sub-solar region to past the terminator. The maximum density varies in time with the solar rotation period, indicating control of the densities by solar ionizing radiation. Electron density increases associated with solar flares were observed. The maximum electron density varies with solar zenith angle as predicted by theory. The altitude profile of electron densities between the maximum density and about 170m altitude is well approximated by a classic Chapman layer. The neutral scale height is close to 10 to 13 km. At altitudes above 180 km the densities deviate from and are larger than inferred by the Chapman layer. At altitudes above the exobase the density decrease was approximated by an exponential function with scale heights between 24 and 65 km. The densities in the top side ionosphere above the exobase tends to be larger than the densities extrapolated from the Chapman layer fitted to the measurements at lower altitudes, implying more efficient upward diffusion above the collision dominated photo equilibrium region.     

太阳风磁帆推进性能数值研究

利用考虑行星际磁场作用的磁流体动力学模型,建立了磁帆三维数值模拟方法,对计算方法的可靠性进行了验证,发现了线圈尾部的磁重联现象,研究了太阳风来流速度、等离子体离子数密度以及攻角对磁帆推进性能的影响。得出以下结论：不同速度、不同离子数密度的太阳风主要通过改变z方向电流的大小改变洛伦兹力,进而影响磁帆的推进性能：太阳风离子数密度恒定时,随着来流速度由30 km/s逐渐增大至75 km/s,z方向电流最大值由4 205 A/m²增至14 709 A/m²,磁帆所受推力由3.39 N增至13.40 N;太阳风来流速度恒定时,随着离子数密度由1.8×10¹⁹ m^-3增大至4.5×10¹⁹ m^-3,z方向电流最大值由6 039 A/m²增至10 585 A/m²,磁帆所受推力由6.62 N增至12.27 N。磁帆攻角变化,主要通过磁场构型的变化影响磁帆推进性能：攻角为0°和90°时的磁层半径分别为0.14 m和0.18 m,...     

Effects of polarization and resolution on SAR ATR

Lincoln Laboratory is investigating the detection and classification of stationary ground targets using high resolution, fully polarimetric, synthetic aperture radar (SAR) imagery. A study is summarized in which data collected by the Lincoln Laboratory 33 GHz SAR were used to perform a comprehensive comparison of automatic target recognition (ATR) performance for several polarization/resolution combinations. The Lincoln Laboratory baseline ATR algorithm suite was used, and was optimized for each polarization/resolution case. Both the HH polarization alone and the optimal combination of HH, HV, and VV were evaluated; the resolutions evaluated were 1 ft/spl times/1 ft and 1 m/spl times/1 m. The data set used for this study contained approximately 74 km/sup 2/ of clutter (56 km/sup 2/ of mixed clutter plus 18 km/sup 2/ of highly cultural clutter) and 136 tactical target images (divided equally between tanks and howitzers).     

Density and Temperature in Wind Tunnels Using Electron Beams

In a paper presented at the last meeting of the International Congress on Instrumentation in Aerospace Simulation Facilities, a method of measuring gas density by radiation scattering was presented. Since that time, the method has been further developed using scattering of 50-keV electrons and has been applied in a wind tunnel using air as a test gas. Test section temperature and density were in the neighborhood of 150°K and 6×10-8 g/cm3. In this application, accuracies better than 1.0 percent appear to be attainable, together with excellent spatial and temporal resolution. The application is described, and comprehensive design data are presented. In addition, the density measurements have been supplemented by measurements of the local rotational temperature, utilizing nitrogen molecular band radiation excited by a second electron beam. Comparisons between the density and temperature measurements and flow properties obtained by standard gas-dynamic calculations are made.     

The Juno Mission

The selection of the Discovery Program InSight landing site took over four years from initial identification of possible areas that met engineering constraints, to downselection via targeted data from orbiters (especially Mars Reconnaissance Orbiter (MRO) Context Camera (CTX) and High-Resolution Imaging Science Experiment (HiRISE) images), to selection and certification via sophisticated entry, descent and landing (EDL) simulations. Constraints on elevation (\({\leq}{-}2.5\ \mbox{km}\) for sufficient atmosphere to slow the lander), latitude (initially 15°S–5°N and later 3°N–5°N for solar power and thermal management of the spacecraft), ellipse size (130 km by 27 km from ballistic entry and descent), and a load bearing surface without thick deposits of dust, severely limited acceptable areas to western Elysium Planitia. Within this area, 16 prospective ellipses were identified, which lie ～600 km north of the Mars Science Laboratory (MSL) rover. Mapping of terrains in rapidly acquired CTX images identified especially benign smooth terrain and led to the downselection to four northern ellipses. Acquisition of nearly continuous HiRISE, additional Thermal Emission Imaging System (THEMIS), and High Resolution Stereo Camera (HRSC) images, along with radar data confirmed that ellipse E9 met all landing site constraints: with slopes <15° at 84 m and 2 m length scales for radar tracking and touchdown stability, low rock abundance (<10 %) to avoid impact and spacecraft tip over, instrument deployment constraints, which included identical slope and rock abundance constraints, a radar reflective and load bearing surface, and a fragmented regolith ～5 m thick for full penetration of the heat flow probe. Unlike other Mars landers, science objectives did not directly influence landing site selection.     

Synthetic Environments for Simulated Missions

Synthetic environments offer Space Flight projects an opportunity to perform rapid, comprehensive, and rigorous modeling of the critical elements of a mission in order to compute quantitative measures of design performance, associated risk, and actual mission utility value. Significantly, these studies can be performed early in the mission cycle. These synthetic terrains are generated on parallel, high-performance computers and served to remote simulations at near-interactive speeds. The terrain creation uses a realistic sequence of physical phenomena such as cratering and dusting with parametric control of features such as surface roughness and rock density. Terrain resolution may be arbitrary but typically ranges from 0.01 to 10 meters. The terrain server has been used for two rover simulations, one using the actual Sojourner autonomy flight code, and the other a more general algorithm. Monte Carlo studies of rover designs interacting with synthetic environments were executed in parallel to quickly compute performance statistics and risk estimates.     

High-Resolution Imaging of Tropospheric Radio Scatterers

A two-dimensional matched filter technique is described for processing ing the signal from a pulsed coherent troposcatter link to obtain high crosspath resolution "maps" showing the relative positions of individual scatterers. For a typical tropolink (station displacement 200 km; midpath beam halfwidth 2 km; wavelength 0.3 meters) crosspath resolution is about 4.5 meters under perfect conditions. Vertical resolution is inversely proportional to scatterer height, but even for wide bandwidth signals is never better than hundreds of meters. Slight velocity mismatches between the signal and filter degrade crosspath resolution considerably so that the scatterers' velocity must be known accurately a priori. Crosspath resolution is relatively insensitive to mismatch in signal and filter record lengths. Random fluctuations of the velocity of a scatterer seriously degrade crosspath resolution. For the typical tropolink parameters and with a 10 m/s scatterer crosspath velocity and a 0.2 m/s standard deviation ion fluctuation the crosspath resolution degrades by an order of magnitude. It is concluded that the matched filter imaging scheme will produce images of individual scatterers if specific atmospheric conditions ions exist. The best results are obtained if the received signal comes from a single scattering layer at a known height, with scatterers moving at a known constant horizontal velocity, with no along-path or vertical components. Such a layer would be observed during night time or early morning when convective and mixing processes are at a minimum.     

激光干涉法在扭摆法测量微冲量中的应用

介绍了激光干涉法测微小转角的原理及测量方法,提出了采用激光干涉测量微冲量的方法,将激光与靶作用产生的微冲量转化为扭摆的转动角度,通过激光干涉法测量此微小转角从而计算出冲量。相同单脉冲能量下,以PVC+2%C为工质,用扭摆法测量了激光与工质作用产生的微冲量,结果表明该测试系统分辨率为2×10-8N.s,量程为2×10-7～0.8×10-5N.s。     

The Descent Imager/Spectral Radiometer (DISR) Experiment on the Huygens Entry Probe of Titan

The payload of the Huygens Probe into the atmosphere of Titan includes the Descent Imager/Spectral Radiometer (DISR). This instrument includes an integrated package of several optical instruments built around a silicon charge coupled device (CCD) detector, a pair of linear InGaAs array detectors, and several individual silicon detectors. Fiber optics are used extensively to feed these detectors with light collected from three frame imagers, an upward and downward-looking visible spectrometer, an upward and downward looking near-infrared spectrometer, upward and downward looking violet phtotometers, a four-channel solar aerole camera, and a sun sensor that determines the azimuth and zenith angle of the sun and measures the flux in the direct solar beam at 940 nm. An onboard optical calibration system uses a small lamp and fiber optics to track the relative sensitivity of the different optical instruments relative to each other during the seven year cruise to Titan. A 20 watt lamp and collimator are used to provide spectrally continuous illumination of the surface during the last 100 m of the descent for measurements of the reflection spectrum of the surface. The instrument contains software and hardware data compressors to permit measurements of upward and downward direct and diffuse solar flux between 350 and 1700 nm in some 330 spectral bands at approximately 2 km vertical resolution from an alititude of 160 km to the surface. The solar aureole camera measures the brightness of a 6° wide strip of the sky from 25 to 75° zenith angle near and opposite the azimuth of the sun in two passbands near 500 and 935 nm using vertical and horizontal polarizers in each spectral channel at a similar vertical resolution. The downward-looking spectrometers provide the reflection spectrum of the surface at a total of some 600 locations between 850 and 1700 nm and at more than 3000 locations between 480 and 960 nm. Some 500 individual images of the surface are expected which can be assembled into about a dozen panoramic mosaics covering nadir angles from 6° to 96° at all azimuths. The spatial resolution of the images varies from 300 m at 160 km altitude to some 20 cm in the last frames. The scientific objectives of the experiment fall into four areas including (1) measurement of the solar heating profile for studies of the thermal balance of Titan; (2) imaging and spectral reflection measurements of the surface for studies of the composition, topography, and physical processes which form the surface as well as for direct measurements of the wind profile during the descent; (3) measurements of the brightness and degree of linear polarization of scattered sunlight including the solar aureole together with measurements of the extinction optical depth of the aerosols as a function of wavelength and altitude to study the size, shape, vertical distribution, optical properties, sources and sinks of aerosols in Titan's atmosphere; and (4) measurements of the spectrum of downward solar flux to study the composition of the atmosphere, especially the mixing ratio profile of methane throughout the descent. We briefly outline the methods by which the flight instrument was calibrated for absolute response, relative spectral response, and field of view over a very wide temperature range. We also give several examples of data collected in the Earth's atmosphere using a spare instrument including images obtained from a helicopter flight program, reflection spectra of various types of terrain, solar aureole measurements including the determination of aerosol size, and measurements of the downward flux of violet, visible, and near infrared sunlight. The extinction optical depths measured as a function of wavelength are compared to models of the Earth's atmosphere and are divided into contributions from molecular scattering, aerosol extinction, and molecular absorption. The test observations during simulated descents with mountain and rooftop venues in the Earth's atmosphere are very important for driving out problems in the calibration and interpretion of the observations to permit rapid analysis of the observations after Titan entry. This revised version was published online in August 2006 with corrections to the Cover Date.     

强激波阵面的非平衡特性研究

利用测量强激波波后N_2~+第一负系(0,0)带和(1,2)带的辐射,对强激波后振动温度历程的进行了测量;利用Langmuir探针技术,在低密度激波管中对强激波后电子数密度历程进行了测量;在弹道靶中进行了激波脱体距离的测量研究.测量和计算结果进行了对比,结果表明:N_2~+B~2∑_u~+态的激发比振动能的激发更快:实验测得的振动温度有明显的周期性振荡;在激波速度7.65km/s～7.85km/s、p_1=1.33Pa、实验段内径0.8m下,实验有效时间只有约6.5μs,实验中的电子数密度不能达到峰值,在约10倍波前自由程的实验有效区域内,电子数密度的测量值与计算值吻合很好.激波脱体距离的测量误差约为5%,是目前国内精度最高的结果.     

City Noise and Its Effect Upon Airborne Antenna Noise Temperatures at UHF

Results of an experimental program to determine the characteristics of city noise and its effect on airborne UHF antennas are presented. Coherent sources of energy from communications equipment, radar, navigational aids, etc. are not included in the analysis. Based upon the experimental data, a model of the industrial noise is presented in which an industrial area is considered as a uniformly distributed source of independent radiators. The magnitude of the power density distribution was computed to be 3×10-18 to 1×10-18 W/m2/Hz over the UHF band for all the East Coast cities measured, with the exception of New York City which was 5 to 6 dB higher. Relations have been derived and curves plotted to compute antenna noise temperature increase due to city noise, based upon the metropolitan area and its range from the aircraft.     

战场环境仿真中的三维地形生成技术研究

在虚拟战场环境的建模技术研究中主要应解决三维地形的生成问题。本文利用Multigen Creator软件来实现三维地形的生成;重点介绍了Creator软件地形转换的四种算法;讨论了在Creator软件中生成地形的过程,并以一个实例为研究区域,建立了一种直观性的、真实性的三维地形。     

高超声速锥柱裙模型边界层转捩的弹道靶实验

为研究高超声速边界层转捩现象、给边界层计算提供可靠的对比数据,在中国空气动力研究与发展中心趟高速弹道靶上开展了锥柱裙模型高超声速边界层转捩的自由飞实验。所采用的锥柱裙模型全长105mm,飞行速度1．94km／s（Ma=5．65）,单位雷诺数4．32×10^7～1．20×10^8m-1。使用激光阴影成像技术,获得了锥柱裙模型边界层转捩和湍流边界层发展的图像,测得的湍流边界层厚度在0．6～2．2mm之间,湍流涡的流向尺寸与边界层厚度的比值介于0．3～0．8之间且沿流向呈下降趋势。实验结果表明：弹道靶实验能够获得给定飞行环境下的高超声速边界层转捩图像,从图像中可以清晰判断转捩位置或区域、测量边界层厚度和分析湍流涡的尺寸。     

Super resolution SAR imaging via parametric spectral estimationmethods

Super resolution synthetic aperture radar (SAR) image formation via sophisticated parametric spectral estimation algorithms is considered. Parametric spectral estimation methods are devised based on parametric data models and are used to estimate the model parameters. Since SAR images rather than model parameters are often used in SAR applications, we use the parameter estimates obtained with the parametric methods to simulate data matrices of large dimensions and then use the fast Fourier transform (FFT) methods on them to generate SAR images with super resolution. Experimental examples using the MSTAR and Environmental Research Institute of Michigan (ERIM) data illustrate that robust spectral estimation algorithms can generate SAR images of higher resolution than the conventional FFT methods and enhance the dominant target features     

Track Initiation of Occasionally Unresolved Radar Targets

In a dense detection environment track-while-scan algorithms will introduce many false tracks when processing is performed on a scan-by-scan basis. The maximum likelihood solution involving all detections on all scans is formulated and evaluated for the initiation problem consisting of false alarms, missed detections, and unresolved detections. A comparison is made between the maximum likelihood solutions including and not including the resolution likelihood and it is shown that the resolution likelihood must be included if the data contain unresolved detections. While the maximum likelihood method (with unresolved detections) does not appear to be implementable in real time without very high speed integrated circuit (VHSIC) technology, it can be used as a standard to which more implementable methods can be compared.     

三向测量技术在深空探测中的应用研究

较详细地介绍了三向测量技术（包括三向测距和三向测速）,阐述使用三向测量的工程背景和重要意义,给出利用三向测量数据进行实时定位的数学推导,并分别对三向测距和三向测速原始数据的误差进行了分析;最后给出在＂嫦娥一号＂试验轨道段采用三向测量技术得到的残差分析结果。结果表明,在未进行站间时间同步的情况下,＂嫦娥一号＂卫星100km×100km环月轨道段三向测距误差约200m,三向测速误差约2cm/s,利用三向测量数据可以单独进行轨道确定,验证了我国后续深空探测中应用三向测量技术的可行性。     

2D C/SiC-ZrB2复合材料的烧蚀性能

用ZrB2微粉对2D C/SiC基体进行改性,研究了化学气相渗透结合浆料浸渍及先驱体浸渍裂解工艺制备2DC/SiC-ZrB2复合材料在氧-乙炔焰和1800℃甲烷风洞环境中的烧蚀行为.结果表明:在氧-乙炔环境中,2D C/SiC-ZrB2的线烧蚀率和质量烧蚀率分别为6.1×10-2 mm/s和1.0×10 -2g/s,相对2D C/SiC复合材料而言,ZrB2微粉并没有提高C/SiC复合材料的抗烧蚀性能.在1800℃甲烷风洞环境中,涂层致密度起主要作用,涂层致密度相同时,复合材料的开气孔率越大,质量烧蚀率越大,ZrB2微粉的渗入对C/SiC复合材料的烧蚀性能影响不大.     

Tradeoff between Picture Element Dimensions and Noncoherent Averaging in Side-Looking Airborne Radar

An experiment was performed to determine the effect on radar image interpretation of: 1) rectangular instead of square pixels, and 2) spatial resolution in the presence of noncoherent averaging. The result is a proof of the hypothesis that interpretability of images is determined by a "spatial-gray-level (SGL) resolution volume" that is the product of the range resolution, the azimuth resolution, and a gray-level resolution. The last is defined as the ratio of the value exceeded 10 percent of the time to that exceeded 90 percent of the time for a chi-square distribution having twice as many degrees of freedom as the number of independent samples averaged. Since the area of the pixel enters, rather than explicit dependence on range or azimuth resolution, rectangular pixels are as interpretable as square pixels having the same area. The SGL accounts for the effect of reduction in fading on interpretability. The numerical interpretability assigned by experienced image interpreters asked to look for specific classes of targets was found to fall exponentially with increasing SGL volume, with a scale determined by the class of target. The experiment showed that, for most of the tasks assigned to the interpreters, the interpretability is reduced to 37 percent for a fully focussed synthetic-aperture radar (SAR) (1-look) for a 10-m (33-ft) square pixel. With an infinite number of samples averaged, the comparable square-pixel dimension is 48 m (157 ft). This is consistent with results obtained using LANDSAT images of about 60-m resolution.     

10. The surface and interior of venus

Present ideas about the surface and interior of Venus are based on data obtained from (1) Earth-based radio and radar: temperature, rotation, shape, and topography; (2) fly-by and orbiting spacecraft: gravity and magnetic fields; and (3) landers: winds, local structure, gamma radiation. Surface features, including large basins, crater-like depressions, and a linear valley, have been recognized from recent ground-based radar images. Pictures of the surface acquired by the USSR's Venera 9 and 10 show abundant boulders and apparent wind erosion.On the Pioneer Venus 1978 Orbiter mission, the radar mapper experiment will determine surface heights, dielectric constant values and small-scale slope values along the sub-orbital track between 50°S and 75°N. This experiment will also estimate the global shape and provide coarse radar images (40–80 km identification resolution) of part of the surface. Gravity data will be obtained by radio tracking. Maps combining radar altimetry with spacecraft and ground-based images will be made. A fluxgate magnetometer will measure the magnetic fields around Venus.The radar and gravity data will provide clues to the level of crustal differentiation and tectonic activity. The magnetometer will determine the field variations accurately. Data from the combined experiments may constrain the dynamo mechanism; if so, a deeper understanding of both Venus and Earth will be gained.     

高精度力值计量巡回标准的研制

摘要根据巡回标准的特殊要求,以应用实例详细介绍了高精度力值计量巡回标准的研制方案。实例中采用McS51单片机、∑-△型A／D芯片、精密参考电源、液晶显示屏模块等,经对数据采集部分的分析估算,得出该标准具有1×10^-4的高精度,分辨率可达满量程的1．2×10^-7。具有结构简单、成本低、接口方便、便携等优点。