The Relativistic Proton Spectrometer (RPS) for the Radiation Belt Storm Probes Mission

The Relativistic Proton Spectrometer (RPS) on the Radiation Belt Storm Probes spacecraft is a particle spectrometer designed to measure the flux, angular distribution, and energy spectrum of protons from ～60 MeV to ～2000 MeV. RPS will investigate decades-old questions about the inner Van Allen belt proton environment: a nearby region of space that is relatively unexplored because of the hazards of spacecraft operation there and the difficulties in obtaining accurate proton measurements in an intense penetrating background. RPS is designed to provide the accuracy needed to answer questions about the sources and losses of the inner belt protons and to obtain the measurements required for the next-generation models of trapped protons in the magnetosphere. In addition to detailed information for individual protons, RPS features count rates at a 1-second timescale, internal radiation dosimetry, and information about electrostatic discharge events on the RBSP spacecraft that together will provide new information about space environmental hazards in the Earth’s magnetosphere.     

行政自由裁量权的道德边界

行政自由裁量权的正确行使,不仅离不开法律控制,而且需要设立道德边界。行政自由裁量权的道德边界,由行政主体在行政自由裁量中应当遵循的道德原则所构成。这样的道德原则主要有:平等裁量原则、公正裁量原则和据实裁量原则。行政自由裁量的道德原则,内化为行政主体的道德信念,就可以使行政主体自觉地控制其自由裁量行为。而公众舆论对于行政自由裁量过程的道德监督,则是实现行政自由裁量的道德原则内化的外部条件。     

纳米复合镍粉雷达吸波涂层研究

采用机械化学法将纳米SiC包覆在镍粉表面制备复合吸波材料,将该材料喷涂在基体上制备吸波涂层,并研究了SiC在复合材料中的含量变化对涂层吸波性能的影响.研究表明,SiC含量为10%时,纳米复合涂层的吸波性能最佳.与镍粉吸波涂层相比,该纳米复合涂层中频段的吸波性能明显提高,发射率小于-5 dB的带宽由7 GHz增加到10.4 GHz,涂层最高吸收值达到-23.4 dB.     

TC11合金高温变形行为及其机理

采用Gleeble-1500热模拟机研究了TC11合金在800～1 050℃、应变速率0.005～5/s条件下的高温变形行为.根据动力学分析,确定了不同温度区间的热激活能和热变形方程.结合变形微观组织观察确定了TC11合金的高温变形机制.结果显示:TC11合金在(α β)两相区和β相区的热变形激活能分别为285.38和141.98 kJ/mol,表明不同温度区间的热变形机理不同;在两相区变形主要发生片状组织的球化,在β相区变形时低应变速率下(0.005～0.05/s)主要发生β相的动态再结晶,高应变速率下(0.05～5/s)主要发生动态回复.研究结果为确定该合金的最佳变形工艺参数提供了理论依据.     

AZ91镁合金搅拌摩擦加工后的组织与性能

采用400rpm-100mm/min,800rpm-100mm/min,800rpm-200mm/min三种工艺参数对铸态AZ91镁合金进行搅拌摩擦加工(FSP)处理,并对合金加工前后的显微组织和拉伸性能及微观断裂机制进行分析。结果表明,经800rpm-100mm/min工艺FSP处理后,合金的显微组织明显细化,延伸率和抗拉强度显著提高,综合拉伸性能最好,且拉伸断口主要表现为韧性断裂的特征。这主要是由于在FSP过程中合金发生动态再结晶,使合金晶粒显著细化及粗大β相的溶解和破碎所致。     

The Electric Antennas for the STEREO/WAVES Experiment

The STEREO/WAVES experiment is designed to measure the electric component of radio emission from interplanetary radio bursts and in situ plasma waves and fluctuations in the solar wind. Interplanetary radio bursts are generated from electron beams at interplanetary shocks and solar flares and are observed from near the Sun to 1 AU, corresponding to frequencies of approximately 16 MHz to 10 kHz. In situ plasma waves occur in a range of wavelengths larger than the Debye length in the solar wind plasma λ _D ≈10 m and appear Doppler-shifted into the frequency regime down to a fraction of a Hertz. These phenomena are measured by STEREO/WAVES with a set of three orthogonal electric monopole antennas. This paper describes the electrical and mechanical design of the antenna system and discusses efforts to model the antenna pattern and response and methods for in-flight calibration.     

The Plasma and Suprathermal Ion Composition (PLASTIC) Investigation on the STEREO Observatories

The Plasma and Suprathermal Ion Composition (PLASTIC) investigation provides the in situ solar wind and low energy heliospheric ion measurements for the NASA Solar Terrestrial Relations Observatory Mission, which consists of two spacecraft (STEREO-A, STEREO-B). PLASTIC-A and PLASTIC-B are identical. Each PLASTIC is a time-of-flight/energy mass spectrometer designed to determine the elemental composition, ionic charge states, and bulk flow parameters of major solar wind ions in the mass range from hydrogen to iron. PLASTIC has nearly complete angular coverage in the ecliptic plane and an energy range from ～0.3 to 80 keV/e, from which the distribution functions of suprathermal ions, including those ions created in pick-up and local shock acceleration processes, are also provided.     

The THEMIS Array of Ground-based Observatories for the Study of Auroral Substorms

The NASA Time History of Events and Macroscale Interactions during Substorms (THEMIS) project is intended to investigate magnetospheric substorm phenomena, which are the manifestations of a basic instability of the magnetosphere and a dominant mechanism of plasma transport and explosive energy release. The major controversy in substorm science is the uncertainty as to whether the instability is initiated near the Earth, or in the more distant >20 Re magnetic tail. THEMIS will discriminate between the two possibilities by using five in-situ satellites and ground-based all-sky imagers and magnetometers, and inferring the propagation direction by timing the observation of the substorm initiation at multiple locations in the magnetosphere. An array of stations, consisting of 20 all-sky imagers (ASIs) and 30-plus magnetometers, has been developed and deployed in the North American continent, from Alaska to Labrador, for the broad coverage of the nightside magnetosphere. Each ground-based observatory (GBO) contains a white light imager that takes auroral images at a 3-second repetition rate (“cadence”) and a magnetometer that records the 3 axis variation of the magnetic field at 2 Hz frequency. The stations return compressed images, “thumbnails,” to two central databases: one located at UC Berkeley and the other at the University of Calgary, Canada. The full images are recorded at each station on hard drives, and these devices are physically returned to the two data centers for data copying. All data are made available for public use by scientists in “browse products,” accessible by using internet browsers or in the form of downloadable CDF data files (the “browse products” are described in detail in a later section). Twenty all-sky imager stations are installed and running at the time of this publication. An example of a substorm was observed on the 23rd of December 2006, and from the THEMIS GBO data, we found that the substorm onset brightening of the equatorward arc was a gradual process (>27 seconds), with minimal morphology changes until the arc breaks up. The breakup was timed to the nearest frame (<3 s) and located to the nearest latitude degree at about ±3^oE in longitude. The data also showed that a similar breakup occurred in Alaska ～10 minutes later, highlighting the need for an array to distinguish prime onset.