Alfvénic Electron Acceleration in Aurora Occurs in Global Alfvén Resonosphere Region

Auroral emission caused by electron precipitation (Hardy et al., 1987, J. Geophys. Res. 92, 12275–12294) is powered by magnetospheric driving processes. It is not yet fully understood how the energy transfer mechanisms are responsible for the electron precipitation. It has been proposed (Hasegawa, 1976, J. Geophys. Res. 81, 5083–5090) that Alfvén waves coming from the magnetosphere play some role in powering the aurora (Wygant et al., 2000, J. Geophys. Res. 105, 18675–18692, Keiling et al., 2003, Science 299, 383–386). Alfvén-wave-induced electron acceleration is shown to be confined in a rather narrow radial distance range of 4–5 R _E (Earth radii) and its importance, relative to other electron acceleration mechanisms, depends strongly on the magnetic disturbance level so that it represents 10% of all electron precipitation power during quiet conditions and increased to 40% during disturbed conditions. Our observations suggest that an electron Landau resonance mechanism operating in the “Alfvén resonosphere” is responsible for the energy transfer.     

冲压发动机燃烧引起激波运动过程一维分析

分析了冲压发动机喷油燃烧引起内流道内正激波运动的机理,采用一维激波捕捉方法,建立了燃油喷入对正激波运动位置影响的一维仿真模型。通过仿真发现:喷入燃油并逐步增大燃油-空气当量比时,正激波逐步向上游运动;燃油-空气当量比越大,正激波越接近进气道喉道;当燃油-空气当量比增大到一定程度时,正激波距离进气道喉道最近,但并未越过喉道;进一步增大燃油-空气当量比,正激波开始向下游回退进一步分析发现:冲压发动机流道及燃烧组织匹配设计直接影响到正激波在流道内的运动位置,需要在设计中格外重视。燃油-空气当量比与激波位置的关系分析可为冲压发动机设计提供一定的理论参考。     

关于BL-代数的implicative滤子的一些结果

通过研究BL-代数的implicative滤子的等价条件,得到了normal滤子与implicative滤子之间的关系,并给出了两个公开问题"一个normal滤子在什么合适条件下成为fantastic滤子?"和"在什么合适的条件下,normal滤子的拓展性成立?"结论成立的一种条件。     

基于离心加速度信息的单站无源测距定位方法

针对只测向（B0）方法具有收敛速度慢、定位误差大等缺点，提出了一种利用角度及其变化率、离心加速度等信息进行单站无源测距定位的新方法。对该方法的单次测距误差进行了分析，经多次测量定位计算机仿真结果表明，该方法比只测角定位方法、角度及其变化率定位方法具有更高的定位精度和更快的收敛速度，并且具有更广的应用范围。     

The role of radial perpendicular diffusion and latitude dependent acceleration along the solar wind termination shock

A numerical model, based on Parker’s transport equation, describing the modulation of anomalous cosmic rays and containing diffusive shock acceleration is applied. The role of radial perpendicular diffusion at the solar wind termination shock, and as the dominant diffusion coefficient in the outer heliosphere, is studied, in particular the role it plays in the effectiveness of the acceleration of anomalous protons and helium when its latitude dependence is changed. It is found that the latitudinal enhancement of radial perpendicular diffusion towards the heliospheric poles and along the termination shock has a prominent effect on the acceleration of these particles. It results in a ‘break’ in the energy spectrum for anomalous protons at ∼6.0 MeV, causing the spectral index to change from E^−1.38 to E^−2.23, but for anomalous helium at ∼3.0 MeV, changing the spectral index from E^−1.38 to E^−2.30. When approaching the simulated TS, the changes in the modulated spectra as they unfold to a ‘steady’ power law shape at energies below 50 MeV are much less prominent as a function of radial distances when radial perpendicular diffusion is increased with heliolatitude.     

Distribution and variability of accelerated electrons at Mars

We investigate accelerated electrons observed by Mars Global Surveyor (MGS), using data from the Electron Reflectometer (ER) instrument. We find three different types of accelerated electron events. Current sheet events occur over regions with weak or no crustal fields, have the highest electron energy fluxes, and are likely located on draped magnetotail fields. Extended events occur over regions with moderate crustal magnetic fields, and are most often observed on closed magnetic field lines. Localized events have the lowest energy fluxes, occur in strong magnetic cusp regions, and are the most likely kind of event to be found on open magnetic field lines. Some localized events have clear signatures of field-aligned currents; these events have much higher electron fluxes, and are preferentially observed on radially oriented open magnetic field lines. Electron acceleration events, especially localized events, are similar in many ways to events observed in the terrestrial auroral zone. However, physical processes related to those found in the terrestrial cusp and/or plasmasheet could also be responsible for accelerating electrons at Mars.     

基于退化模型的失效机理一致性检验方法

有效的加速试验必须保证产品的失效机理不变。针对加速退化试验(ADT)可靠性建模的特点,提出了一种基于退化模型的失效机理一致性检验方法。以基于随机过程和基于退化轨迹拟合的退化模型为例,通过加速系数的2种等效定义分别建立了模型参数与失效机理不变的内在联系,进一步推导出其参数在不同应力下须满足的关系。在合理假定检验样本服从正态分布的基础上,利用t统计量对样本的一致性进行检验。通过2个ADT实例验证了所提检验方法的合理性与可行性。     

某型民用飞机电源系统负加速度试飞研究

首先对民用飞机电源系统负加速度试飞进行简要说明,提出民用飞机电源系统负加速度试飞的原因和目的。其次对电源系统负加速度试飞条件、试飞方法和试飞程序进行说明。对电源系统负加速试飞结果进行分析评估,表明电源系统设计是满足设计要求和民用航空标准要求的。最后对负加速度试飞中注意事项进行了详细说明,为其它机型飞机进行负加速度试飞提供借鉴。     

RT-11燃油调节器加速性不稳定原因分析

介绍了某型发动机的RT-11燃油调节器加速性不稳定、起飞状态燃油供油量停滞的情况,分析了产生故障的原因和故障机理,并提出了修理中的改进措施。     

The Role of Magnetic Reconnection in CME Acceleration

Observations carried out from the coronagraphs on board space missions (LASCO/SOHO, Solar Maximum and Skylab) and ground-based facilities (HAO/Mauna Loa Observatory) show that coronal mass ejections (CMEs) can be classified into two classes based on their kinematics evolution. These two classes of CMEs are so-called fast and slow CMEs. The fast CME starts with a high initial speed that remains more or less constant; it is also called the constant-speed CME. On the other hand, the slow CME starts with a low initial speed, but shows a gradual acceleration; it is also called the accelerated and slow CME. Low and Zhang [Astrophys. J. 564, L53–L56, 2002] suggested that these two classes of CMEs could be a result of a difference in the initial topology of the magnetic fields associated with the underlying quiescent prominences. A normal prominence magnetic field topology will lead to a fast CME, while an inverse quiescent prominence results in a slow CME, because of the nature of the magnetic reconnection processes. In a recent study given by Wu et al. [Solar Phys. 225, 157–175, 2004], it was shown that an inverse quiescent prominence magnetic topology also could produce a fast CME. In this study, we perform a numerical MHD simulation for CMEs occurring in both normal and inverse quiescent prominence magnetic topology. This study demonstrates three major physical processes responsible for destabilization of these two types of prominence magnetic field topologies that can launch CMEs. These three initiation processes are identical to those used by Wu et al. [Solar Phys. 225, 157–175, 2004]. The simulations show that both fast and slow CMEs can be initiated from these two different types of magnetic topologies. However, the normal quiescent prominence magnetic topology does show the possibility for launching a reconnection island (or secondary O-line) that might be thought of as a “CME’’.