The French-Soviet ‘ARAKS’ experiment

In 1975, a rocket borne electron gun experiment will be achieved in Kerguelen Islands (South Indian Ocean), as a result of a cooperation between Soviet and French scientists. The gun will inject into the magnetosphere large currents (0.5 and 1 A) of high energy electrons (15 and 27 keV) with different initial pitch angles ( 0°, 70, 140°). A nose cone will be ejected at great distance ( 10 km) in front of the rocket, equipped mainly with radio wave receivers, both electric and magnetic, in the frequency range from 0 to 5 MHz, in order to study the wave particle interactions which will be induced by the beam. Optical and radioelectric observations will be performed in the conjugate area, in the district of Arkhangelsk (U.S.S.R.). During one of the two flights (launched in the magnetic meridian) attention will be focused on the wave particle interactions which are expected to be stronger when the beam is injected along the magnetic field line. The second flight, which will be launched towards the east, is attempted to study the azimuthal drift of the injected electrons and to derive some conclusions concerning the DC electric field, integrated over the line of force which joins the two conjugate points (L = 3.7). During both flights the energy and pitch angle distribution of atmospherically backscattered electrons will be studied.We describe the experiment and give the results of some preliminary computations which have been made by the different experimenters in order to predict the amplitude of the expected phenomena. A discussion is made of the respective ability for electron beam injection and cold plasma injection to artificially induce strong particle precipitation.On leave from Groupe de Recherches Ionosphériques, CNET, 92131 Issy-les-Moulineaux, France.     

The Freja wave and plasma density experiment

The Wave Experiment, F4, on the Swedish/German satelliteFreja, is designed to measure the electric wave fields up to 4 MHz, the magnetic wave fields up to 16 kHz and the plasma density and its relative variations up to 2 kHz. Six wave signals and four density probe signals can be measured simultaneously. The wave forms of all signals are transmitted to ground without any analysis onboard. The limited TM allocation does not allow continuous sampling of the wave signals, so normally the measurements are made in snapshots of various lengths dependent on sampling frequency, etc. Continuous sampling can be made for shorter time periods by using a 6 Mbyte memory as a buffer.     

The comptel experiment on the NASA Gamma-Ray Observatory

The imaging Compton telescope COMPTEL will be flown on the NASA Gamma-Ray Observatory at the beginning of the next decade. The instrument with its wide field of view and improved angular resolution will provide the first sky survey at MeV energies, as well as deep studies of galactic and extragalactic gamma-ray point sources and diffuse emission. The hardware preparations are close to completion, with calibrations to be done in 1987 prior to integration of the instrument onto the observatory carrying 3 other gamma ray detectors.     

The W-band data collection experiment of the DAVID mission

The data collection experiment (DCE) of the scientific mission DAVID (DAta and Video Interactive Distribution) of the Italian Space Agency (ASI) will pioneer the use of the W-band for telecommunications experiments. In particular the collection of high volumes of data from remote or virtually remote sites will be achieved through the exploitation of a W-band link in a time window of a few minutes per satellite pass. The experiment will hence demonstrate the capability of the W-band channel to be used reliably for a telecommunication link. At the same time, the experiment will provide useful elements for the characterisation of the W-band channel, in order to be able to design properly future operational systems working at W-band.     

The 22 GHz resource sharing experiment of the DAVID mission

The resource sharing experiment (RSE) of the DAVID (DAta and Video Interactive Distribution) multiexperiment mission of the Italian Space Agency (ASI) is described. The experiment envisages adaptively varying the robustness of signals down-transmitted, to a set (16) of Earth terminals by acting on their coding and spreading. During the DAVID satellite passes, each terminal determines autonomously its signal-to-noise ratio (SNR) and transmits it to a central station which, by using this information, works out the parameters for the global system optimization and indicates, in real time, to the terminals which code and despreading factor they must utilize to receive the part of the signal addressed to them.     

预习型实验课程网络选课系统的实现

主要介绍物理实验中心自主研发的预习型网络选课系统的开发和应用。为了调动学生预习实验的积极性,该系统把物理实验的网络选课系统、实验预习系统、网络仿真实验等结合起来,使得学生在选课之前,必须要进行实验预习和通过预习测试,从根本上确保学生实验预习的质量,从而使实验教学管理工作更加规范、标准和高效,保证实验教学质量。该系统主要是基于网络数据库平台进行开发,运用了多媒体课件技术,面向互联网开放。     

Galileo Probe Nephelometer experiment

The objective of the Nephelometer Experient aboard the Probe of the Galileo mission is to explore the vertical structure and microphysical properties of the clouds and hazes in the atmosphere of Jupiter along the descent trajectory of the Probe (nominally from 0.1 to > 10 bars). The measurements, to be obtained at least every kilometer of the Probe descent, will provide the bases for inferences of mean particle sizes, particle number densities (and hence, opacities, mass densities, and columnar mass loading) and, for non-highly absorbing particles, for distinguishing between solid and liquid particles. These quantities, especially the location of the cloud bases, together with other quantities derived from this and other experiments aboard the Probe, will not only yield strong evidence for the composition of the particles, but, using thermochemical models, for species abundances as well. The measurements in the upper troposphere will provide ground truth data for correlation with remote sensing instruments aboard the Galileo Orbiter vehicle. The instrument is carefully designed and calibrated to measure the light scattering properties of the particulate clouds and hazes at scattering angles of 5.8°, 16°, 40°, 70°, and 178°. The measurement sensitivity and accuracy is such that useful estimates of mean particle radii in the range from about 0.2 to 20 can be inferred. The instrument will detect the presence of typical cloud particles with radii of about 1.0 , or larger, at concentrations of less than 1 cm³.Deceased.     

GMTI along-track interferometry experiment

Synthetic aperture radar (SAR) along track interferometry (ATI) has been used extensively to measure ocean surface currents. Given its ability to measure small velocities (/spl sim/ 10 cm/s) of relatively radar-dark water surfaces, there is great potential that this technique can be adapted for ground moving target indication (GMTI) applications, particularly as a method for detecting very slow targets with small radar cross-sections. In this paper we describe preliminary results from an ATI GMTI experiment. The SAR data described herein were collected by the dual-frequency NASA/JPL airborne radar in its standard dual-baseline ATI mode. The radar system imaged a variety of control targets including a pickup truck, sport utility vehicles, passenger cars, a bicycle, and pedestrians over multiple flight passes. The control targets had horizontal velocities of less than 5 m/s. The cross-sections of the targets were not purposely enhanced, although the targets' reflectivities may have been affected by the existence of the GPS equipment used to record the targets' positions. Single-look and multiple-look interferograms processed to the full azimuth resolution were analyzed. In the data processed to date, all of the targets were observed by visual inspection in at least one of the four combinations of dual-frequency, dual-baseline interferometric data. This extremely promising result demonstrates the potential of ATI for GMTI applications.     

Charged-particle telescope experiment on Clementine

The charged-particle telescope (CPT) onboard the Clementine spacecraft measured the fluxes of energetic protons emitted in solar energetic particle events. Protons in the energy range from 10 to 80 MeV were of greatest interest for radiation effects such as total dose and single event upsets. Energetic electrons were also of interest for spacecraft charging and their contribution to total dose. The lower-energy CPT electron channels (25-500 keV) were mainly of geophysical interest. While orbiting the moon, the CPT observed the wake created by the moon when it blocked the flow of energetic particles in the magnetotail region. The CPT provided opportunities to observe energetic electron bursts during magnetic storms and magnetospheric substorms. CPT data are particularly useful in multispacecraft studies of interplanetary disturbances and their interaction with the magnetosphere. The proton channels on the CPT provided data on solar energetic protons and storm-time protons associated with the passage of an interplanetary shock at 0903 UT on Feb. 21, 1994. Results are compared with those from GOES-7, SAMPEX, and GEOTAIL.     

Galileo Net Flux Radiometer experiment

The Galileo Net Flux Radiometer (NFR) is a Probe instrument designed to measure the vertical profile of upward and net radiation fluxes in five spectral bands spanning the range from solar to far infrared wavelengths. These unique measurements within Jupiter's atmosphere, from which radiative heating and cooling profiles will be derived, will contribute to our understanding of Jovian atmospheric dynamics, to the detection of cloud layers and determination of their opacities, and to the estimation of water vapor abundance. The NFR uses an array of pyroelectric detectors and individual bandpass filters in a sealed detector package. The detector package and optics rotate as a unit to provide chopping between views of upward and downward radiation fluxes. This arrangement makes possible the measurement of small net fluxes in the presence of large ambient fluxes. A microprocessor-controlled electronics package handles instrument operation.     

Galileo Photopolarimeter/Radiometer experiment

The Photopolarimeter/Radiometer (PPR) is a remote sensing instrument on the Galileo Orbiter designed to measure the degree of linear polarization and the intensity of reflected sunlight in ten spectral channels between 410 and 945 nm to determine the physical properties of Jovian clouds and aerosols, and to characterize the texture and microstructure of satellite surfaces. The PPR also measures thermal radiation in five spectral bands between 15 and 100 m to sense the upper tropospheric temperature structure. Two additional channels which measure spectrally integrated solar and solar plus thermal radiation are used to determine the planetary radiation budget components. The PPR photopolarimetric measurements utilize previously flown technology for high-precision polarimetry using a calcite Wollaston prism and two silicon photodiodes to enable simultaneous detection of the two orthogonal polarization components. The PPR radiometry measurements are made with a lithium tantalate pyroelectric detector utilizing a unique arrangement of radiometric stops and a scene/space chopper blade to enable a warm instrument to sense accurately the much colder scene temperatures.     

Galileo Probe Mass Spectrometer experiment

The Galileo Probe Mass Spectrometer (GPMS) is a Probe instrument designed to measure the chemical and isotopic composition including vertical variations of the constituents in the atmosphere of Jupiter. The measurement will be performed by in situ sampling of the ambient atmosphere in the pressure range from approximately 150 mbar to 20 bar. In addition batch sampling will be performed for noble gas composition measurement and isotopic ratio determination and for sensitivity enhancement of non-reactive trace gases.The instrument consists of a gas sampling system which is connected to a quadrupole mass analyzer for molecular weight analysis. In addition two sample enrichment cells and one noble gas analysis cell are part of the sampling system. The mass range of the quadrupole analyzer is from 2 amu to 150 amu. The maximum dynamic range is 10⁸. The detector threshold ranges from 10 ppmv for H₂O to 1 ppbv for Kr and Xe. It is dependent on instrument background and ambient gas composition because of spectral interference. The threshold values are lowered through sample enrichment by a factor of 100 to 500 for stable hydrocarbons and by a factor of 10 for noble gases. The gas sampling system and the mass analyzer are sealed and evacuated until the measurement sequence is initiated after the Probe enters into the atmosphere of Jupiter. The instrument weighs 13.2 kg and the average power consumption is 13 W.The instrument follows a sampling sequence of 8192 steps and a sampling rate of two steps per second. The measurement period lasts appropriately 60 min through the nominal pressure and altitude range.     

贝叶斯方法在导弹武器系统试验评估中的应用

介绍了贝叶斯方法及其与仿真技术的结合运用,指出贝叶斯小子样理论对导弹武器装备发展的重要性,着重分析研究了贝叶斯方法在导弹武器系统性能评定中的应用.     

供油压力对齿轮箱传递扭矩影响的试验研究

目前大功率齿轮箱仍采用强制供油的方式进行润滑,其供油压力越大润滑程度越好,但同时产生的传递扭矩损失也越大。针对试验过程中供油压力不稳定问题,开展了供油压力对齿轮箱传递扭矩影响的试验研究,建立了齿轮箱扭矩损失随转速、供油压力的数据模型和扭矩修正方法,并在小功率压气机上进行了试验验证。结果表明,该扭矩修正模型能消除供油压力不稳定造成的齿轮箱传递扭矩差异的影响,可在一定程度上提高小功率压气机低速性能试验评估的准确性。     

薄板坯连铸结晶器电磁制动的热模拟实验

本文以Sn作为模拟合金，测定了有无电磁制动条件下结晶器的二维速度分布。实验结果表明；电磁制动对于减轻液面波动，改善薄板坯连铸结晶器内的流场有明显效果。此项工作对于板坯连铸结晶器电磁制动器的设计和工艺参数的确定具有一定的参考价值。     

Spartan 201 white light coronagraph experiment

A white light coronagraph was launched into orbit aboard the space shuttle OV 103 (Discovery) on 7 April 1993. This device was one of two instruments included in the SPARTAN 201-1 payload, a completely autonomous sub-satellite deployed from the shuttle for a period of about 47 hours. The WLC system is an externally occulted coronagraph system which incorporates a rotating half-wave plate polarimeter, and the image data is used to infer the brightness, the polarized brightness and the degree of polarization of the white light emission from the solar corona. These data are in turn used to infer estimates of the K- and F-coronal brightnesses and density distributions. We shall present preliminary results of the electron density estimate in the coronal streamer and hole region and describe the methods employed.affiliated to USRA