振动传感器的微加速度动态校准

阐述了高灵敏度振动传感器在超低频微小加速度下进行动态校准的校准装置工作原理、校准方法 ,分析了其校准不确定度。该装置采用曲率半径为 10m的虚拟摆结构 ,从较强的环境干扰噪声中利用数字滤波技术成功地拾检微弱振动信号 ,使微小标准加速度获得复现。该装置可在 (0 .0 0 1～ 0 .1)Hz超低频率范围内和 (1× 10 -6～ 1× 10 -2 )m s2 微小加速度范围内实现高准确度激光绝对校准和比较法校准 ,其校准不确定度达 0 .5%。     

翼型测力天平的研制

为研究翼型结冰状态下的载荷变化规律，对翼型进行测力实验。研制一台三分量翼型测力天平。天平设计的突出难点为设计载荷极不匹配，阻力测量载荷很小。设计时，针对翼型载荷的特点，采用片梁组合方式测量阻力，四柱梁测量法向力及俯仰力矩，并采用有限元方法对结构进行了验证计算。主要介绍天平的设计、校准及应用情况。     

Fe/O Ratios in Interplanetary Shock Accelerated Particles

It is widely accepted that diffusive shock acceleration is an important process in the heliosphere, in particular in producing the energetic particles associated with interplanetary shocks driven by coronal mass ejections. In its simplest formulation shock acceleration is expected to accelerate ions with higher mass to charge ratios less efficiently than those with lower mass to charge. Thus it is anticipated that the Fe/O ratio in shock-accelerated ion populations will decrease with increasing energy above some energy. We examine the circumstances of five interplanetary shocks that have been reported to have associated populations in which Fe/O increases with increasing energy. In each event, the situation is complex, with particle contributions from other sources in addition to the shock. Furthermore, we show that the Fe/O ratio in shock-accelerated ions can decrease even when the shock is traveling through an Fe-rich ambient ion population. Thus, although shock acceleration of an Fe-rich suprathermal population has been proposed to explain large Fe-rich solar particle events, we find no support for this proposal in these observations.     

Oxygen line mapping of SN 1006 with Suzaku

SN 1006 is one of the supernova remnants (SNRs) with relatively low-temperature electrons, considering the young age of just 1000 years. We carried out SN 1006 mapping observations with the X-ray Imaging Spectrometers (XIS) and the Hard X-ray Detector (HXD) onboard Suzaku, the fifth Japanese X-ray satellite. Thanks to the excellent spectral resolution of XIS in the soft X-ray band, H-like and He-like oxygen emission lines were clearly detected, and we could make a map of the line intensity, and as well as a flux and the photon index of nonthermal component. We found that these parameters have spatial dependences from region to region in the SNR; the north region is bright in nonthermal, while dim in thermal; the east region is bright in both nonthermal and thermal; the inner region shows dim nonthermal and bright thermal emission. The photon index is the smallest in the north region.     

一种四层次样本轮换方法——基于多阶段季度调查的研究

四阶段抽样季度调查需要实施四层次样本轮换，在构造四层次样本轮换方法时主要应考虑三个问题，一是相邻两个季度四级单元的样本拼配率，二是相邻两年相同季度四级单元的样本拼配率，三是保证各级单元的样本拼配率在轮换过程中保持不变。如果一级单元、二级单元、三级单元和四级单元的样本轮换模式分别为32in、16in、8in和2-2-2（4），则这四个样本轮换模式就可组合成一种四层次样本轮换方法。该方法可以应用于中国劳动力调查的四层次样本轮换中。     

New evidence for strong non-thermal effects in Tycho’s supernova remnant

For the case of Tycho’s supernova remnant (SNR), we present the relation between the blast wave and contact discontinuity radii calculated within the nonlinear kinetic theory of cosmic ray (CR) acceleration in SNRs. It is demonstrated that these radii are confirmed by recently published Chandra measurements which show that the observed contact discontinuity radius is very close to the shock radius. Therefore a consistent explanation of these observations can be given in terms of efficient CR acceleration which makes the medium more compressible.     

Solar Sources of Heliospheric Energetic Electron Events—Shocks or Flares?

Electrons with near-relativistic (E≳30 keV, NrR) and relativistic (E≳0.3 MeV) energies are often observed as discrete events in the inner heliosphere following solar transient activity. Several acceleration mechanisms have been proposed for the production of those electrons. One candidate is acceleration at MHD shocks driven by coronal mass ejections (CMEs) with speeds ≳1000 km s⁻¹. Many NrR electron events are temporally associated only with flares while others are associated with flares as well as with CMEs or with radio type II shock waves. Since CME onsets and associated flares are roughly simultaneous, distinguishing the sources of electron events is a serious challenge. On a phenomenological basis two classes of solar electron events were known several decades ago, but recent observations have presented a more complex picture. We review early and recent observational results to deduce different electron event classes and their viable acceleration mechanisms, defined broadly as shocks versus flares. The NrR and relativistic electrons are treated separately. Topics covered are: solar electron injection delays from flare impulsive phases; comparisons of electron intensities and spectra with flares, CMEs and accompanying solar energetic proton (SEP) events; multiple spacecraft observations; two-phase electron events; coronal flares; shock-associated (SA) events; electron spectral invariance; and solar electron intensity size distributions. This evidence suggests that CME-driven shocks are statistically the dominant acceleration mechanism of relativistic events, but most NrR electron events result from flares. Determining the solar origin of a given NrR or relativistic electron event remains a difficult proposition, and suggestions for future work are given.     

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.     

基于数值模拟的燃气舵轴向位置优化分析

为了优化燃气舵的安装位置,应用fluent软件对燃气舵三维湍流流场结构进行了分析,在此基础上就燃气舵安装位置对燃气舵流场的影响进行了数值模拟.通过数值模拟得到燃气舵在不同轴向位置、耳片长度和舵偏角下绕流流场的复杂波系结构,绘制了燃气舵在不同舵偏角下升力的变化曲线,给出了燃气舵可以提供的升力参量随舵偏角度变化的规律.通过分析,确定了燃气舵的轴向安装位置,数值模拟和实验结果相符.     

磁悬浮框架飞轮磁轴承技术研究与发展现状

对磁悬浮框架飞轮(MSGFW)和高精度磁轴承研究现状及其未来发展进行了详细阐述。根据转子悬浮力类型，将磁悬浮框架飞轮分为磁阻力构型、洛伦兹力构型和混合力构型，并结合三种构型论述了国内外框架飞轮的发展过程。在此基础上，对球面磁阻力磁轴承和洛伦兹力磁轴承进行了详细介绍，并结合磁路图分析其工作原理，比较了同类磁轴承的优劣。展望了磁悬浮框架飞轮与高精度磁轴承的未来发展方向，指出高动态响应检控共位平动球面磁阻力磁轴承，标准磁悬浮动量球和磁悬浮控制敏感球是磁悬浮框架飞轮的研究重点。