Coronal fast wave trains of the decimetric type IV radio event observed during the decay phase of the June 6, 2000 flare

The 22 min long decimetric type IV radio event observed during the decay phase of the June 6, 2000 flare simultaneously by the Brazilian Solar Spectroscope (BSS) and the Ond?ejov radiospectrograph in frequency range 1200–4500 MHz has been analyzed. We have found that the characteristic periods of about 60 s belong to the long-period spectral component of the fast wave trains with a tadpole pattern in their wavelet power spectra. We have detected these trains in the whole frequency range 1200–4500 MHz. The behavior of individual wave trains at lower frequencies is different from that at higher frequencies. These individual wave trains have some common as well as different properties. In this paper, we focus on two examples of wave trains in a loop segment and the main statistical parameters in their wavelet power and global spectra are studied and discussed.     

功能梯度压电材料层状结构中的SH波

基于线性压电弹性理论,利用传递矩阵法,分析了功能梯度压电材料层状结构中的SH波传播特性,研究了压电梯度覆盖层中初始应力对SH波传播的影响。压电覆盖层的材料性能如弹性、压电、介电系数和密度沿厚度方向呈梯度变化。数值分析结果表明,适当的材料梯度分布,可使SH波倾向于沿覆盖层表面传播,由此能够获得更好的机电耦合性能;同时,初始应力使得波传播的相速度减小,但增大了机电耦合系数。文中的分析方法和结论,对固体火箭发动机超声探伤及其压电类传感器的研制和选择有一定的参考意义。     

毫米波宽带低副瓣波导缝隙阵列天线设计

本文提出了一种毫米波宽带低副瓣波导缝隙阵列天线。该天线分为上下两层,利用下层的功分器和反相器使电磁波从上层的辐射波导的两端向中心进行馈电,激励12个非均匀波导缝隙辐射单元。该天线呈中心对称结构,结构紧凑,并使得天线的方向图具有稳定性。在辐射波导中引入二阶短路金属阶梯,并且阵列的辐射单元采用非连续的双层缝隙,拓展了天线的工作带宽。所提出的加载二阶金属阶梯双层缝隙阵列天线的阻抗带宽达到16.3%(35.35~41.55 GHz),峰值增益为16 dBi,工作频带内天线的增益下降低于2.5 dBi,副瓣电平低于-20 dB。     

A comparative and numerical study of effects of gravity waves in small miss-distance and miss-time GPS radio occultation temperature profiles

The Global Positioning System (GPS) Radio Occultation (RO) technique has global coverage and is capable of generating high vertical resolution temperature profiles of the upper troposphere and lower stratosphere with sub-Kelvin accuracy and long-term stability, regardless of weather conditions. In this work, we take advantage of the anomalously high density of occultation events at the eastern side of the highest Andes Mountains during the initial mission months of COSMIC (Constellation Observing System for Meteorology, Ionosphere and Climate). This region is well-known for its high wave activity. We choose to study two pairs of GPS RO, both containing two occultations that occurred close in time and space. One pair shows significant differences between both temperature profiles. Numerical simulations with a mesoscale model were performed, in order to understand this discrepancy. It is attributed to the presence of a horizontal inhomogeneous structure caused by gravity waves.     

Gravity wave momentum flux generation close to mid-latitude Andes in mesoscale simulations of late 20th and 21st centuries

Adequate representations of diverse dynamical processes in general circulation models (GCM) are necessary to obtain reliable simulations of the present and the future. The parameterization of orographic gravity wave drag (GWD) is one of the critical components of GCM. It is therefore convenient to evaluate whether standard orographic GWD parameterizations are appropriate. One alternative is to study the generation of gravity waves (GW) with horizontal resolutions that are higher than those used in current GCM simulations. Here we assess the seasonal pattern of topographic GW momentum flux (GWMF) generation for the late 20th and 21st centuries in a downscaling using the Rossby Centre regional atmospheric model under the Intergovernmental Panel on Climate Change A1B emission conditions. We focus on one of the world’s strongest extra-tropical GW zones, the Andes Mountains at mid-latitudes in the Southern Hemisphere. The presence of two GCM sub-grid scale structures locally contributing to GWMF (one positive and one negative) is found to the East of the mountains. For the late 21st century the strength of these structures during the GW high season increases around 23% with respect to the late 20th century, but the GWMF average over GCM grid cell scales remains negative and nearly constant around −0.015 Pa. This constitutes a steady significant contribution during GW high season, which is not related to the GWMF released by individual sporadic strong GW events. This characteristic agrees with the fact that no statistically significant variation in GWMF at source level has been observed in recent GCM simulations of atmospheric change induced by increases in greenhouse gases.     

考虑粘性相互作用的跨音速机翼分析

本文将一些已有的三维全位势方程计算方法和一种三维积分边界层方法作了弱相互作用的耦合计算。计算了三种机翼并与已有的试验数据作了比较。     

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.     

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.     

Assessment of Two Turbulence Models and Some Compressibility Corrections for Hypersonic Compression Comers by High-order Difference Schemes

The Spalart-Allmaras (S-A) turbulence model,the shear-stress transport (SST) turbulenee model and their compressibility corrections are revaluated for hypersonic compression corner flows by using high-...     

突跃型与平滑型斜爆震波起爆机制数值模拟

采用带有化学反应的Euler方程,对突跃型与平滑型2种形态的斜爆震波(ODW)在起爆机制和结构特点等方面的差异进行了研究.结果表明:斜激波(OSW)后是否存在亚声速区是判定斜爆震形态的依据.当波后火焰抬升斜激波面使得亚声速区存在时,横向激波与三波点结构就会出现并形成突跃型斜爆震.当波后所有区域皆为超声速区时,波后火焰燃烧无法影响到上游激波面,则会形成平滑型斜爆震.通过斜激波关系式给出了横向激波形成所需的临界斜激波角度,只有当斜激波角度大于此临界角度时才能形成突跃型斜爆震波,反之则形成平滑型斜爆震波.