V.L.A. observations of flare build-up in coronal loops

Very Large Array (V.L.A.) measurements at 20 cm wavelength map emission from coronal loops with second-of-arc angular resolution at time intervals as short as 3.3 seconds. The total intensity of the 20 cm emission describes the evolution and structure of the hot plasma that is detected by satellite X-ray observations of coronal loops. The circular polarization of the 20 cm emission describes the evolution, strength and structure of the coronal magnetic field. Preburst heating and magnetic changes that precede burst emission on time scales of between 1 and 30 minutes are discussed. Simultaneous 20 cm and soft X-ray observations indicate an electron temperature $\text{T}{}_{\mathrm{e}}\textcolor{red}{}\text{2.5 × 10}{}^7\text{K}$ and electron density $\text{N}{}_{\mathrm{e}}\textcolor{red}{}\text{10}{}^{10}\text{cm}{}^{\mathrm{?3}}$ during preburst heating in a coronal loop that was also associated with twisting of the entire loop in space. We also discuss the successive triggering of bursts from adjacent coronal loops; highly polarized emission from the legs of loops with large intensity changes over a 32 MHz change in observing frequency; and apparent motions of hot plasma within coronal loops at velocities V > 2,000 kilometerspersecond.     

Multiple wavelength observations of flaring active regions

We present observations of flaring active regions with the Very Large Array (V.L.A. at 6 cm and 20 cm wavelengths) and the Westerbork Synthesis Radio Telescope (W.S.R.T. at 6 cm wavelength). These are compared with photospheric magnetograms (Meudon) and with Hα and offband Hα photographs (Big Bear and Ottawa River Solar Observatories). The 6 cm radiation of these active regions marks the legs of dipolar loops which have their footpoints in lower-lying sunspots. The intense, million degree radiation at 6 cm lies above sunspot umbrae in coronal regions where the longitudinal magnetic field strength H_? = 600 Gauss and the height above the sunspot umbrae h = 3.5±0.5 × 10⁹ cm. Circularly polarized horseshoe structures at 6 cm ring the sunspot umbrae. The high degree of circular polarization (?_c = 95%) of the horseshoes is attributed to gyroresonant emission above sunspot^? penumbrae. The 20 cm radiation of these active regions exhibits looplike coronal structures which extend across regions of opposite magnetic polarity in the underlying photosphere. The 20 cm loops are the radio wavelength counterparts of the X-ray coronal loops. We infer semilengths L = 5 × 10⁹ cm, maximum electron temperatures T_e(max) = 3 × 10⁶ K, emission measures ∫N_e²d$\text{l}$ = 10²⁸ cm^?5, and electron densities N_e = 10⁹ cm^?3 (or pressures p = 1 dyn cm^?2) for the 20 cm bremsstrahlung. A total of eight solar bursts were observed at 6 cm or 20 cm wavelength with second-of-arc angular resolution. The regions of burst energy were all resolved with angular sizes between 5″ and 30″, brightness temperatures between 2 × 10⁷ K and 2 × 10⁸ K, and degrees of circular polarization between 10% and 90%. The impulsive phase of the radio bursts are located near the magnetic neutral lines of the active regions, and between the flaring Hα kernels which mark the footpoints of magnetic loops. In one case there was preburst heating in the coronal loop in which a burst occurred. Snapshot maps at 10 s intervals reveal interesting burst evolution including rapid changes of circular polarization and an impulsive burst which was physically separated from both the preburst radio emission and the gradual decay phase of the burst.     

论大学生思想政治教育新媒体利用的机遇与挑战

在技术发展、教育时空领域扩大、党和政府政策支持、师生媒介素养提升的条件下,大学生思想政治教育新媒体利用迎来了一系列的机遇。与此同时,也遭遇了以下挑战：信息风暴带来了大学生思想政治教育新媒体利用的难以分辨和选择;虚拟空间交往方式的异化产生了大学生思想政治教育新媒体利用的隐痛;依赖的强化造就了大学生思想政治教育新媒体利用过程中的控制和反控制;身心健康受影响,成为大学生思想政治教育新媒体利用的忧患。     

焊接残余应力超声无损检测技术

基于声弹性理论,针对天然气输送管道焊缝残余应力检测问题,本文提出了一种检测新技术,并研制残余应力超声检测系统。该系统采用一发一收的探头分布方式,传感器沿着管道直焊缝放置,传感器吸附于管道外壁并在管道表面及亚表面激发出临界折射纵波,测得管道外壁沿着直焊缝处的焊接残余应力分布情况,并且经过实验验证该系统对管道焊接残余应力测量的可靠性。针对温度变化较大环境下的曲面材料的残余应力检测问题,提出了温度补偿技术和曲率补偿技术。     

航空发动机复杂型面罩子钣充液成形技术

利用先进的钣材冲压计算机仿真技术对零件成形中的关键问题进行了研究,并通过先进的充液成形技术进行了实际零件的成形试验,试验的结果与模拟结果基本一致。最后应用模拟得到的成形参数,利用钣充液成形工艺成形出了合格的零件。     

航空发动机性能参数联合RBFPN和FAR预测

排气温度是最能反映航空发动机运行状态的性能参数之一.对连续飞行班次的起飞排气温度裕度(EGTM,Exhaust Gas Temperature Margin)参数进行预测分析,有助于判知航空发动机将来的工作性能,为预防和排除故障提供充分的时间和决策依据.在依据具有非线性、非平稳特征的起飞EGTM历史监测值序列构建预测模型时,基于奇异值分解滤波算法提出了一种联合径向基函数预测网络(RBFPN,Radial Basis Function Prediction Networks)和函数系数自回归模型(FAR,Functional-coefficient Auto Regressive model)的预测方案,充分发挥RBFPN和FAR在预测EGTM参数值变动趋势成分和随机成分的各自优势,使其互为补充,协同处理.实验结果表明该联合预测方案能够有效抑制RBFPN或FAR单独采用时所呈现出的不足,提高预测性能.     

基于"序列相对贴近度"的组合预测权值分配

在时间序列的组合预测权值分配问题上,为克服传统的均方误差倒数加权、熵权和最优化方法之不足,从预测值序列与评价样本序列间的贴近性出发,提出新方法综合衡量单一参与模型的适用性,并据此分配权值.详细给出了序列相对贴近度(SRND,Sequence Relative Nearness Degree)及与之相关的"序列趋势关联度"和"尺度区间熵"的概念,并提出基于SRND的权值分配方法.将SRND权值分配方法应用于航空发动机排气温度裕度参数时间序列的联合自回归滑动平均模型、函数系数自回归模型和径向基函数网络预测,有效地提高了预测准确度,获得优于均方误差倒数加权和熵权方法的组合性能,且运算量远小于最优化方法.     

带肋变截面回转通道内沿程有效压力分布特性的实验研究

以某型航空发动机的实际涡轮叶片内部的带肋变截面180°回转通道为研究对象,以实验的方法分别研究了带90°直肋和带60°斜肋的通道内的流体流动的特性。根据研究问题的特点,定义了壁面有效压力及局部有效压力系数,并得到了其沿程分布及两种通道内有效压力系数的经验公式。实验发现,对于带90°直肋和带60°斜肋的矩形回转通道沿程有效压力的分布趋势基本一致,由于流道截面积的不规则变化,导致有效压力有沿程逆增现象。      

我国计量行业法规政策和发展趋势分析

计量是实现单位统一、保证量值准确可靠的活动，关系国家安全、国计民生。为夯实计量基础、提升计量能力，抓住计量事业发展的新机遇，本文从行业法规政策、计量发展趋势等方面开展相关研究，为从事计量管理和技术研究工作的人员提供参考。     

Effect of surface roughness on microwave brightness temperature from lunar surface: Numerical analysis with a hybrid method

A hybrid method, combining the radiative transfer theory and the method of moments (MoM), is proposed to study the potential effect of the lunar surface roughness on the microwave brightness temperature. The total upward emission reaching the lunar surface from below media is calculated by the radiative transfer theory, and then the brightness temperature is obtained by weighting the bidirectional transmission coefficients which is computed using the MoM. The method is validated by both flat and rough surface models with analytic solutions. With the hybrid method, brightness temperatures from simulated lunar model are calculated and compared to those from a flat layered model. The comparisons show that the effect of rough surface on brightness temperature cannot be ignored and also depends on many other factors, such as observation angle and polarizations. For vertical polarization, an optimal observation angle may exist to reduce the effect of surface roughness. These results indicate that the knowledge of lunar surface roughness is important in microwave remote sensing to the Moon and may probably provide a guide to lunar projects in future.