Galileo Probe Measurements of D/H and 3He/4He in Jupiter's Atmosphere

The Galileo Probe Mass Spectrometer measurements in the atmosphere of Jupiter give D/H = (2.6 ± 0.7) × 10-5 3He/4He = (1.66 ± 0.05) × 10-4These ratios supercede earlier results by Niemann et al. (1996) and are based on a reevaluation of the instrument response at high count rates and a more detailed study of the contributions of different species to the mass peak at 3 amu. The D/H ratio is consistent with Voyager and ground based data and recent spectroscopic and solar wind (SW) values obtained from the Infrared Spectroscopic Observatory (ISO) and Ulysses. The 3He/4He ratio is higher than that found in meteoritic gases (1.5 ± 0.3) × 10-4. The Galileo result for D/H when compared with that for hydrogen in the local interstellar medium (1.6 ± 0.12) × 10-5 implies a small decrease in D/H in this part of the universe during the past 4.55 billion years. Thus, it tends to support small values of primordial D/H - in the range of several times 10-5 rather than several times 10-4. These results are also quite consistent with no change in (D+3He)/H during the past 4.55 billion years in this part of our galaxy.     

Balloon altitude studies of southern hemisphere hard X-ray sources by the Imperial College-University of Tasmania-INPE collaboration

Hard X-ray balloon altitude measurements with a 1600 cm² phoswich array are described. Data from observations on Sco X-1, GX1+4, GX5−1, Nova Oph. 1977, SMC X-1, SS433, IC 4329A and MR 2251-178 are presented. The role of Comptonisation in X-ray production for Sco X-1 and GX1+4 is discussed.     

用推力矢量控制技术改进超声速飞行器空气动力特性

为了提高某超声速飞机的空气动力学效率和机动性能，本文采用低阶的三维板块法和DATCOM半经验公式，在亚声速和超声速条件下，对不同马赫数和迎角情况计算了基本气动外形的飞机空气动力学特性、表面压力分布以及最大升力。此外还开发了一套软件以实现由引进的先进气动操纵面（如鸭翼等）控制的二维推力矢量技术。试验结果表明：气动操纵面结合推力矢量技术能够产生足够的低头力矩，且有能力满足高度机动飞行时的稳定性要求。此外，不论是亚声速还是超声速飞行，气动操纵面均可以提高气动效率5％-6％。     

利用几何遗传方法优化前缘翼根延伸的外形以增强飞行器升力系数和机动性

为了提高所选定飞行器模型的机动性,采用了一种标准遗传算法设计前缘翼根延伸(LEX).同时使用一种由三维低阶板方法结合DATCOM方法半经验公式的改进方法预测复杂外形飞行器(机身 机翼 尾翼)的空气动力载荷和最大升力系数.结果表明,在前缘翼根存在的情况下,升力系数在马赫数为0.4～0.8时提升了20.5%～15.3%,在马赫数为1.2时提升了6.8%,在马赫数为0.2～0.95之间升力系数最大值提升了9.5%～15%.在1～5 km的高度亚音速飞行时,其回转率得到了6.6%～8.0%的提升.     

基于鲁棒自适应控制策略的混合型步进电机低速伺服控制性能

针对混合型步进电机低速运行状态下脉动转矩较大的特点,应用鲁棒自适应控制策略来设计其低速伺服控制器,以实现高精度的跟踪控制性能.首先,根据混合型步进电机转矩形成的机理,揭示了其固有的脉动转矩对低速运动控制产生不利影响的动力学特征,并将它归结为两种结构不确定性,便于控制器的设计;其次,采取标准的自适应控制及其鲁棒化设计思想,借助于μ-修整策略来实现相应的控制律,确保脉动转矩的最大化补偿及伺服系统低速跟踪控制满足高性能的要求;最后对所建立的低速跟踪控制系统的性能进行了试验评估,并与作者前期的工作进行了比较,试验结果验证了其有效性与可行性.     

An empirical model of the plasma environment around Mercury

Since the flyby observations by Mariner 10 in 1974 and 1975, Mercury has been one of the most interesting objects for space physics and planetary exploration. The MESSENGER and BepiColombo missions now plan to revisit this planet. In order to design plasma instruments for the BepiColombo mission, we have estimated electron and ion fluxes around Mercury with an empirical model, which has been developed for the Earth’s magnetotail. The solar wind data needed as input parameters are derived from Helios observations. The result shows that our predicted electron fluxes at aphelion agree well with the Mariner-10 data. It is also noted that ion instruments must cover a very wide dynamic range of proton fluxes. However, the applicability of the Earth’s magnetospheric model to Mercury is, in itself, an important issue for comparative magnetospheric studies.     

Non-Thermal Processes in Cosmological Simulations

Non-thermal components are key ingredients for understanding clusters of galaxies. In the hierarchical model of structure formation, shocks and large-scale turbulence are unavoidable in the cluster formation processes. Understanding the amplification and evolution of the magnetic field in galaxy clusters is necessary for modelling both the heat transport and the dissipative processes in the hot intra-cluster plasma. The acceleration, transport and interactions of non-thermal energetic particles are essential for modelling the observed emissions. Therefore, the inclusion of the non-thermal components will be mandatory for simulating accurately the global dynamical processes in clusters. In this review, we summarise the results obtained with the simulations of the formation of galaxy clusters which address the issues of shocks, magnetic field, cosmic ray particles and turbulence.     

Great solar bursts of October 19, 22 and 23, 1989

Itapetinga measurements at 48 GHz with the multibeam technique are used to determine the relative position of solar burst centroid of emission with high spatial accuracy and time resolution. For the Great Bursts of October 19,22, 1989, with a large production of relativistic particles, and October 23, it is suggested that, at 48 GHz, the bursts might have originated in more then one source in space and time. Additionally the October 19 and 22 Ground Level Events exhibited very unusual intensity-time profiles including double component structures for the onset phase. The Bern observatory spectral radio emission data show a strong spectral flattening typical for large source inhomogeneties. The interpretation for this is that large solar flares are a superposition of a few strong bursts (separated both in space and time) in the same flaring region.     

WIND/3DP and Nancay radioheliographobservations of solar energetic electron events

Initial results of a combined study of electron events using the 3DP experiment on the WIND spacecraftand the Nançay Radioheliograph (NRH) are presented. A total of 57 electron events whose solar release time could be inferred from WIND/3DP observations occurred during NRH observing times. In 40 of them a distinct signature was detected in maps at decimetric and metric wavelengths (dm-m-λ) taken by the NRH. These events are equally distributed among two categories: (1) Electron release together with dm-m-λ bursts of a few minutes duration: these events are also accompanied by decametric-hectometric type III bursts seen by WAVES/WIND. They correspond to the well-known impulsive electron events. (2) Electron release during long duration (several tens of minutes) dm-m-λ emission: the electrons are most often released more than ten minutes after the start of the radio event. In the majority of cases the dm-m-λ radio source changes position, size, and/or intensity near the time of electron release.