金星表面THz遥感探测

从“金星快车可见光与红外热成像光谱仪（VIRTIS）载荷成功地实现了对金星表面辐射探测”事实出发,利用高分辨率传输分子光谱数据库（HITRAN）,仿真验证了金星大气模型相适应的近红外大气窗口,从而分析并获取了金星 THz 大气窗口。与此相适应,从实现金星地表全天候遥感探测科学目标出发,系统阐述了金星大气 THz窗口下探测的优势,提出多功能金星遥感构想。     

金星热气球与环境红外透射特性的仿真研究

考虑到搭建用于模拟金星环境的实验室具有相当的困难并存在一定的危险,首先通过计算机仿真模拟金星的 大气环境,然后在该环境下仿真热气球从脱离所有的平台到最终稳定在某一高度上进行探测的整个运动过程。 通过比较不同参数下的热气球仿真结果,可以更好地辅助热气球的设计。最后提出建立地球与金星等效水平路 程关系的新思路,用以仿真红外辐射在金星大气中的透射特性,为红外载荷系统的设计提供参考信息,也为后续金 星热气球及其红外载荷系统的研究提供一个新的方向。     

Pioneer Venus Orbiter Neutral Gas Mass Spectrometer Experiment

The Pioneer Venus Orbiter Neutral Mass Spectrometer (ONMS) is designed to measure the vertical and horizontal density variations of the major neutral constituents in the upper atmosphere of Venus. The mass spectrometer sensor includes a retarding potential ion source, hyperbolic quadrupole rod analyzer, and electron multiplier detector. The supporting electronic system consists of hybrid integrated circuits to reduce weight and power. The ONMS instrument was launched aboard the Pioneer Venus Orbiter on May 20, 1978, and turned on in orbit around Venus on December 4, 1978. It has operated flawlessly for over a Venus year (243 earth days) and has returned data of the composition of the major constituents in the Venus atmosphere between the altitudes of 150 and 350 km.     

The Pioneer Venus Orbiter Plasma Analyzer Experiment

The plasma analyzer experiment on the Pioneer Venus Orbiter was designed to determine the basic characteristics of the plasma environment of Venus and the nature of the solar wind interaction at Venus. The plasma analyzer experiment is an electrostatic energy-per-unit charge (E/Q) spectrometer which measures ions and electrons. There is a curved plate electrostatic analyzer system with multiple collectors. The experiment obtains the three dimensional plasma distribution function. Some of the scientific objectives of the instrument are briefly discussed, the general characteristics of the experiment are summarized, and some of the analyses based on the data are presented.     

The planetary exploration program

The U. S. program for space exploration of the planets began with the Mariner 2 flyby of Venus in 1962. Since then a series of Mariners have gone to Mercury and Mars, in addition to Venus. Pioneer-class spacecraft have flown through the asteroid belt and have passed by Jupiter. The Viking mission carried Out a spectacularly successful series of measurements at Mars. These past missions will be followed shortly by recently launched Voyager flybys of Jupiter and Saturn in 1977 and by Pioneer probes and orbiter to Venus in 1978. These missions have stressed exploration. Now there are two additional goals involving the well-being of Man which are looming on the space horizon.     

Pioneer Venus Occultation Radio Science Data Generation

Previous to the Pioneer Venus Orbiter mission, occultation radio science data were generated at the Deep Space Stations of NASA's Deep Space Network via the analog recording of the baseband frequency output signal of a relatively wide bandwidth open-loop receiver. Signal digitization was a separate and subsequent operation at the Jet Propulsion Laboratory. During Pioneer Venus Orbiter radio science operations, the open-loop receiver baseband frequency output signal bandwidth was substantially reduced. This was made possible by programming the open-loop receiver first local oscillator with the predicted Doppler frequency profile. In addition, the receiver output signal was digitized and recorded directly on computer compatible magnetic tape in real time. Initial results obtained with this new process, referred to as ?real-time bandwidth reduction,? during the prime Pioneer Venus Orbiter mission, compare very favorably to results obtained with the previous occultation system.     

Pioneer Venus Sounder Probe Particle Size Spectrometer

The Pioneer Venus Sounder Probe Particle Size Spectrometer measured the particle size and number density in the atmosphere of Venus from 66 km to the surface. This instrument performs particle size measurements over a 0.5 to 500-?m size range using a combination of shadowgraph imaging and light scattering techniques. Size resolution is approximately ±10 percent of size with 100-400-m vertical spacial resolution. The instrument features a laser-fed optical system incorporating a complex beam-splitting multipath imaging optical system.     

Pioneer Venus Sounder Probe Solar Flux Radiometer

The Solar Flux Radiometer aboard the Pioneer Venus Sounder Probe operated successfully during its descent through the atmosphere of Venus. The instrument measured atmospheric radiance over the spectral range from 400 to 1800 nm as a function of altitude. Elevation and azimuthal measurements on the radiation field were made with five optical channels. Twelve filtered Si and Ge photovoltaic detectors were maintained near 30°C with a phase-change material. The detector output currents were processed with logarithmic transimpedance converters and digitized with an 11-bit A/D converter. Atmosphetic sampling in both elevation and azimuth was done according to a Gaussian integration scheme. The serial output data averaged 20 b/s, included housekeeping (sync, spin period, sample timing and mode). The data were used to determine the deposition of solar energy in the atmosphere of Venus between 67 km and the surface along with upward and downward fluxes and radiances with an altitude resolution of several hundred meters. The results allow for more accurate modelling of the radiation balance of the atmosphere than previously possible.     

Pioneer Venus Multiprobe Entry Telemetry Recovery

The Entry Phase of the Pioneer Venus Multiprobe Mission involved data transmission over only a two-hour span. The criticality of recovery of those two hours of data, coupled with the fact that there were no radio signals from the Probes until their arrival at Venus, dictated unique telemetry recovery approaches on the ground. The result was double redundancy, use of spectrum analyzers to aid in rapid acquisition of the signals, and development of a technique for recovery of telemetry data without the use of real-time coherent detection which is normally employed by all other NASA planetary missions.     

The electromagnetic propagation characteristics of venus and mars

The information available about Mars and Venus and their atmospheres has been examined to determine the electro-magnetic propagation characteristics of each planet. Consideration of some preliminary model atmospheres [6] indicates that the electro-magnetic propagation effective radius of Venus is between 7400 and 13 900 km. Other models are discussed which give even larger effective radii and lead to the limit of a plane surface. The troposphere of Mars, because of its low density, was shown to have essentially no effect on the propagation loss between points on the surface or near the surface. An examination of the knowledge of the dielectric constants and conductivities of the surface revealed considerable uncertainties, Measured values of the dielectric constant are between 2.2 and 7.1 for the Venusian surface. The conductivity probably is 10^-3mhos/meter or less for both the Venusian and Martian surfaces if they have compositions similar to dry terrestrial soil. No measurement of the dielectric constant of the surface of Mars has been published. Mars and Venus are strongly believed to have ionospheres in their atmospheres, but only crude estimations are available for the electron densities and the altitudes of these ionospheres.     

High-gain backup antenna design for Pioneer Venus Orbiter spacecraft

The development and performance is described of a high-gain antenna designed to serve on the Pioneer Venus Orbiter spacecraft as a backup to the principal high-gain antenna unit in the unlikely event the mechanically despun antenna mechanism malfunctioned. The final design, a center-fed standing wave array of six sleeve dipoles enclosed in a fiber glass radome, performed successfully, as did all the antennas, on the Pioneer Orbiter spacecraft which was launched on May 20, 1978, as part of the Pioneer Venus mission. Photographs of experimental models giving details of design and construction are included, as well as graphs showing measured pattern and impedance matching characteristics of the subject antenna.     

Pioneer Venus Sounder Probe Gas Chromatograph

The Pioneer Venus Sounder Probe gas chromatograph (GC) instrument's design logic, construction, function, and data processing are discussed.     

A New Paphiopedilum Orchid Database and Its Recognition Using Convolutional Neural Network

Wireless Personal Communications - This paper discusses a visual recognition system, for identifying the Pa-phiopedilum orchid, often called the Venus slipper. The dataset consists of 100 sample...     

Thermal radio radiation from the moon and planets

Thermal radio radiation has been observed from the moon, Mercury, Venus, Mars, Jupiter, and Saturn. The most important result of the observations is the discovery that the temperature at the surface of Venus, beneath the clouds, is greater than600degK. The thermal radio radiation from the moon comes from beneath the surface and gives information about the temperature distribution and variation which can be interpreted in terms of the physical characteristics of the subsurface material. This also should apply to the planets with thin atmospheres. The thermal radio radiation from Jupiter should give information about the temperature distribution in the extensive absorbing atmosphere, but the intensity of the thermal radiation is confused by the nonthermal radiation of the radiation belts and cannot be accurately specified until more observational data are available.     

Pioneer Venus Orbiter Fluxgate Magnetometer

The fluxgate magnetometer on the Pioneer Venus orbiter spacecraft is described. Special features include gradiometer operation, on board despinning, a floating point processor and variable Nyquist filters. Initial operations have been entirely successful.     

多波长激光治愈298例太田痣临床分析

采用美国科以人公司维纳斯多波长激光治疗太田痣983例,其中治愈298例。本文着重介绍治疗方法、皮损程度与治愈所需时间的关系。     

The AMPTE/CCE Plasma Wave Investigation

The payload of the Charge Composition Explorer includes a small plasma wave instrument that is actually a modified version of the flight spare from the Pioneer Venus Orbiter. In this report the instrument characteristics are summarized and the in-flight performance is briefly described.     

Pioneer Venus Orbiter Radar Mapper: Design And Operation

The Radar Mapper Experiment, carried abroad the Pioneer Venus Orbiter spacecraft, is designed to obtain a near-global picture of the topography, meter-scale surface slopes and reflectivity of Venus. Constraints imposed by the choice of orbit limit radar coverage to a latitude band lying between 74°N and 61°S completely around the planet. In addition to the altimetry objectives, the experiment seeks an image of the radar scattering properties of the surface at oblique incidence. Sensitivity limits the imaged region to a band around the planet lying between 45°N and 10°S. Altimetric error is less than 200 m; altimetric surface ?footprint? size varies from about 10 km in diameter at a spacecraft altitude of 200 km, to 50 km at a maximum altitude of 4700 km. Imaging resolution varies from 20 to 40 km, depending on spacecraft altitude.     

Spacecraft studies of planetary surfaces using bistatic radar

Spaceborne transmitters have been used in bistatic geometries for a number of planetary surface studies including inference of topography, Fresnel reflectivity, and RMS surface slopes on the Moon, Mars, and Venus. For the Moon and Mars in particular, the bistatic geometry has enabled remote probing in regions and under conditions not obtainable with Earth-based radar systems, yielding information about surface characteristics and properties on scales of centimeters to hundreds of meters that complements monostatic radar observations. A new generation of planetary spacecraft now provides opportunities for further experiments, including more nearly complete definition of the surface scattering function and, possibly, imaging. Targets of interest include the polar regions of Venus (by Magellan) and Mars (by Mars Observer), the enigmatic icy Galilean satellites of Jupiter (by Galileo), and Saturn's largest moon Titan (by Cassini)     

物联网架构与应用

本文首先分析了物联网的基本概念、与CPS之异同,分析了物联网的三层基础架构及EPC体系架构,在此基础上提出了Venus物联网应用平台及在宝钢水处理监控系统中应用。