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.     

The DAVID mission in the heritage of the SIRIO and ITALSAT satellites

The DAta and Video Interactive Distribution (DAVID) mission belongs to the Small Missions for Science and Technology Programme of the Italian Space Agency (ASI) and is aimed at pioneering the use of the W-band channel for telecommunications experiments. Furthermore, it envisages the test of a novel technique, for an optimal sharing of the satellite resources, among a grid of Earth terminals, that could be usefully exploited in future W-band operational systems.     

The Toroidal Imaging Mass-Angle Spectrograph (TIMAS) for the polar mission

The science objectives of the Toroidal Imaging Mass-Angle Spectrograph (TIMAS) are to investigate the transfer of solar wind energy and momentum to the magnetosphere, the interaction between the magnetosphere and the ionosphere, the transport processes that distribute plasma and energy throughout the magnetosphere, and the interactions that occur as plasma of different origins and histories mix and interact. In order to meet these objectives the TIMAS instrument measures virtually the full three-dimensional velocity distribution functions of all major magnetospheric ion species with one-half spin period time resolution. The TIMAS is a first-order double focusing (angle and energy), imaging spectrograph that simultaneously measures all mass per charge components from 1 AMU e^–1 to greater than 32 AMU e^–1 over a nearly 360° by 10° instantaneous field-of-view. Mass per charge is dispersed radially on an annular microchannel plate detector and the azimuthal position on the detector is a map of the instantaneous 360° field of view. With the rotation of the spacecraft, the TIMAS sweeps out very nearly a 4 solid angle image in a half spin period. The energy per charge range from 15 eV e^–1 to 32 keV e^–1 is covered in 28 non-contiguous steps spaced approximately logarithmically with adjacent steps separated by about 30%. Each energy step is sampled for approximately 20 ms;14 step (odd or even) energy sweeps are completed 16 times per spin. In order to handle the large volume of data within the telemetry limitations the distributions are compressed to varying degrees in angle and energy, log-count compressed and then further compressed by a lossless technique. This data processing task is supported by two SA3300 microprocessors. The voltages (up to 5 kV) for the tandem toroidal electrostatic analyzers and preacceleration sections are supplied from fixed high voltage supplies using optically controlled series-shunt regulators.     

全球首位自费旅游者的太空之旅(上)

蒂托是美藉意大利人，他经营着资产超百亿美元的大型公司。今年４月２３日，蒂托花２０００万美元到国际空间站俄罗斯太空舱进行了７天的旅行     

全球首位自费旅游者的太空之旅(下)

蒂托花２０００万美元到太 空旅游，成为世界上首位登上太空的富翁，实现了到太空旅游的梦想。远程记者招待会在莫斯科夏令时时间５月４日１１时１０分，蒂托首次在国际空间站上举行了远程记者招待会，讲述了他的新奇感受。 在俄罗斯地面飞行控制中心的雷达显示屏上，蒂托对记者说，太空生活超乎想象。习以为常的生活模式已全然发生了变化，这里完全是另外一个世界，处处都让人感到惊讶。这里的物品，不论大小均需加以固定，以避免自由飘浮。在确保不磕碰的前提下，宇航员可以自由自在地“滑翔”。在专业宇航员看来，这或许没有什么特别的，…     

全球首位自费旅游者的太空之旅(中)

由于俄罗斯宇航局据理 争取，蒂托终于要实规太空旅游了。激动的心情２００１年４月中旬，蒂托在接受路透社采访时说：“我的这趟太空之行经受了多次挫折，但好在现在看来我已度过了这些困难，我很高兴不久我就要在发射台上了。我现在无法想象升入太空的那一刻是什么样子，或许我会很紧张，甚至有点神经质，但我可以肯定的是我的这趟太空游的经历将是不可思议的，我为此付出的所有努力也是值得的。对这趟旅行的风险，我已做好充分的思想准备。可以说，确实含有风险，但成功率也很高，我不担心出什么差错。出错总是可能的，但６１岁时，即使…     

Medium energy neutral atom (MENA) imager for the IMAGE mission

The Medium Energy Neutral Atom (MENA) imager was developed in response to the Imaging from the Magnetopause to the Aurora for Global Exploration (IMAGE) requirement to produce images of energetic neutral atoms (ENAs) in the energy range from 1 to 30 keV. These images will be used to infer characteristics of magnetospheric ion distributions. The MENA imager is a slit camera that images incident ENAs in the polar angle (based on a conventional spherical coordinate system defined by the spacecraft spin axis) and utilizes the spacecraft spin to image in azimuth. The speed of incident ENAs is determined by measuring the time-of-flight (TOF) from the entrance aperture to the detector. A carbon foil in the entrance aperture yields secondary electrons, which are imaged using a position-sensitive Start detector segment. This provides both the one-dimensional (1D) position at which the ENA passed through the aperture and a Start time for the TOF system. Impact of the incident ENA on the 1D position-sensitive Stop detector segment provides both a Stop-timing signal and the location that the ENA impacts the detector. The ENA incident polar angle is derived from the measured Stop and Start positions. Species identification (H vs. O) is based on variation in secondary electron yield with mass for a fixed ENA speed. The MENA imager is designed to produce images with 8°×4° angular resolution over a field of view 140°×360°, over an energy range from 1 keV to 30 keV. Thus, the MENA imager is well suited to conduct measurements relevant to the Earth's ring current, plasma sheet, and (at times) magnetosheath and cusp.     

High energy neutral atom (hena) imager for the IMAGE mission

The IMAGE mission will be the first of its kind, designed to comprehensively image a variety of emissions from the Earth's magnetosphere, with sufficient time resolution to follow the dynamics associated with the development of magnetospheric storms. Energetic neutral atoms (ENA) emitted from the ring current during storms are one of the key emissions that will be imaged. This paper describes the characteristics of the High Energy Neutral Atom imager, HENA. Using pixelated solid state detectors, imaging microchannel plates, electron optics, and time of flight electronics, HENA is designed to return images of the ENA emitting regions of the inner magnetosphere with 2 minute time resolution, at angular resolution of 8 degrees or better above the energy of 50 keV/nucleon. HENA will also image separately the emissions in hydrogen, helium, and oxygen above 30 keV/nucleon. HENA will reject energetic ions below 200 keV/charge, allowing ENA images to be returned in the presence of ambient energetic ions. HENA images will reveal the distribution and the evolution of energetic ion distributions as they are injected into the ring current during geomagnetic storms, as they drift about the Earth on both open and closed drift paths, and as they decay through charge exchange to pre-storm levels. Substorm ion injections will also be imaged, as will the regions of low altitude, high latitude ion precipitation into the upper atmosphere.     

The Radiation Belt Storm Probes (RBSP) and Space Weather

Following the launch and commissioning of NASA’s Radiation Belt Storm Probes (RBSP) in 2012, space weather data will be generated and broadcast from the spacecraft in near real-time. The RBSP mission targets one part of the space weather chain: the very high energy electrons and ions magnetically trapped within Earth’s radiation belts. The understanding gained by RBSP will enable us to better predict the response of the radiation belts to solar storms in the future, and thereby protect space assets in the near-Earth environment. This chapter details the presently planned RBSP capabilities for generating and broadcasting near real-time space weather data, discusses the data products, the ground stations collecting the data, and the users/models that will incorporate the data into test-beds for radiation belt nowcasting and forecasting.     

The Analyzer of Space Plasmas and Energetic Atoms (ASPERA-3) for the Mars Express Mission

The general scientific objective of the ASPERA-3 experiment is to study the solar wind – atmosphere interaction and to characterize the plasma and neutral gas environment with within the space near Mars through the use of energetic neutral atom (ENA) imaging and measuring local ion and electron plasma. The ASPERA-3 instrument comprises four sensors: two ENA sensors, one electron spectrometer, and one ion spectrometer. The Neutral Particle Imager (NPI) provides measurements of the integral ENA flux (0.1–60 keV) with no mass and energy resolution, but high angular resolution. The measurement principle is based on registering products (secondary ions, sputtered neutrals, reflected neutrals) of the ENA interaction with a graphite-coated surface. The Neutral Particle Detector (NPD) provides measurements of the ENA flux, resolving velocity (the hydrogen energy range is 0.1–10 keV) and mass (H and O) with a coarse angular resolution. The measurement principle is based on the surface reflection technique. The Electron Spectrometer (ELS) is a standard top-hat electrostatic analyzer in a very compact design which covers the energy range 0.01–20 keV. These three sensors are located on a scanning platform which provides scanning through 180^∘ of rotation. The instrument also contains an ion mass analyzer (IMA). Mechanically IMA is a separate unit connected by a cable to the ASPERA-3 main unit. IMA provides ion measurements in the energy range 0.01–36 keV/charge for the main ion components H⁺, He⁺⁺, He⁺, O⁺, and the group of molecular ions 20–80 amu/q. ASPERA-3 also includes its own DC/DC converters and digital processing unit (DPU).     

3D Coronal structures and their evolutions measured by Stereoscopy,consequences for Space Weather and the STEREO mission

We are discussing methods of stereoscopic 3D reconstruction of coronal loops structures. In our most sophisticated method we fit loops observed with SOHO/EIT to a set of shape parameters including the internal twist of the loops field lines. We define this twist as the number of turns of the field line around a torus axis between the footpoints of the loops. Twist numbers of the order 0–2 are observed. We observe the emergence of an Active Region with twisted loops which detwist as they expand. The same correlation between detwisting and expansion is observed with filaments in relation to CME formations. On longer time scale, loops seem to accumulate twist, perhaps due to differential rotation. Rapid losses of twist temporarily correlate with flares. From our analysis, we expect that the internal twist of coronal structures will play an important role for the space weather forecast. This revised version was published online in August 2006 with corrections to the Cover Date.     

International Space Station (ISS)-a star is born

The impact of systems engineering approach, materials science developments and robotics on further developments of Space Stations is discussed     

基于时空观的企业社会责任探讨

对企业社会责任演进过程进行了探讨,指出企业承担社会责任大致经过了端倪初显、利润最大化和利益相关者三个阶段,目前企业社会责任有泛化的趋势。企业承担社会责任应考虑企业的发展阶段、企业的规模及企业产品销售或服务的地域性,过分强调企业承担最高层次的社会责任对企业乃至于对社会都会造成损害。