Solar Gamma-Ray Spectroscopy

Interactions of ions accelerated in solar flares produce gamma-ray lines and continuum and neutrons. These emissions contain a rich set of observables that provides information about both the accelerated ions and the environment where the ions are transported and interact. Ion interactions with the various nuclei present in the ambient medium produce gamma-ray lines at unique energies. How abundance information is extracted from the measurements is discussed and results from analyses of a number of solar flares are presented. The analyses indicate that the composition of the ambient gas where the ions interact (typically at chromospheric densities) is different from that of the photosphere and more like the composition of the corona, exhibiting low-FIP elemental enhancements that may vary from flare to flare. Evidence for increased Ne/O and the photospheric ³He abundance is also discussed.     

Observations of loops and prominences

We review recent observations by the Yohkoh-SXT in collaboration with other spacecraft and ground-based observatories of coronal loops and prominences. These new results point to problems that SoHO will be able to address. With a unique combination of rapid-cadence digital imaging (32 s full-disk and 2 s partial-frame images), high spatial resolution (2.5 arcsec pixels), high sensitivity (EM 10⁴² cm^–3), a low-scatter mirror, and large dynamic range, SXT can observe a vast range of targets on the Sun. Over the first 21 months of Yohkoh operations, SXT has taken over one million images of the corona and so is building up an invaluable long-term database on the large-scale corona and loop geometry. The most striking thing about the SXT images is the range of loop sizes and shapes. The active regions are a bright tangle of magnetic field lines, surrounded by a network of large-scale quiet-Sun loops stretching over distances in excess of 10⁵ km. The cross-section of most loops seems to be constant. Loops displaying significant increase in the ratio of the footpoint to loop-top diameter () are the exception, not the rule, implying the presence of widespread currents in the corona.All magnetic structures show changes. Time scales range from seconds to months. The question of how these structures are formed, become filled with hot plasma, and are maintained is still open. While we see the propagation of brightenings along the length of active-region loops and in X-ray jets with velocities of several hundred km/s, much higher velocities are seen in the quiet Sun. In XBP flares, for example, velocities of over 1000 km/s are common. Active-region loops seem to be in constant motion, moving slowly outward, carrying plasma with them. During flares, loops often produce localized brightenings at the base and later at the apex of the loop. Quiescent filaments and prominences have been observed regularly. Their coronal manifestation seems to be an extended arcade of loops overlying the filament. Reliable alignment of the ground-based data with the X-ray images make it possible to make a detailed intercomparison of the hot and cold plasma structures over extended periods. Hence we are able to follow the long-term evolution of these structures and see how they become destabilized and erupt.     

Langmuir Turbulence and Solar Radio Bursts

Langmuir waves and turbulence resulting from an electron beam-plasma instability play a fundamental role in the generation of solar radio bursts. We report recent theoretical advances in nonlinear dynamics of Langmuir waves. First, starting from the generalized Zakharov equations, we study the parametric excitation of solar radio bursts at the fundamental plasma frequency driven by a pair of oppositely propagating Langmuir waves with different wave amplitudes. Next, we briefly discuss the emergence of chaos in the Zakharov equations. We point out that chaos can lead to turbulence in the source regions of solar radio emissions. This revised version was published online in August 2006 with corrections to the Cover Date.     

激光捷联惯导系统角增量输入姿态算法

在对经典理想角增量输入的圆锥算法分析总结基础上,提出并推导了更为合适的经典角增量输入圆锥算法通式.在对经典理想角增量与实际工程滤波角增量的圆锥响应对比分析基础上,推导了滤波角增量输入圆锥补偿算法的补偿系数和误差主项通式.最后,利用文中讨论的理想角增量输入和滤波角增量输入圆锥补偿算法,结合激光陀螺惯性导航系统的频谱特性进行了大量的仿真验证.仿真结果表明,文中讨论的角增量圆锥算法有效,能显著提高激光陀螺捷联惯性导航系统的姿态精度.     

基于优化最小二乘支持向量机的襟翼趋势预测

将最小二乘支持向量机(LS-SVM)应用于飞机襟翼状态趋势研究。首先,通过分析飞机襟翼故障与襟翼动作耗时参数的关系,提出了利用动作耗时趋势来确定该系统未来状态的方法。然后,使用最小二乘支持向量机建立耗时回归预测模型,采用最终预报误差(FPE)准则确定回归模型嵌入维数,提出了自适应网格搜索法,优化最小二乘支持向量机的建模参数,从而实现比现有方法精度高,泛化性能好的预测模型。训练和测试样本取自飞行数据记录系统(QAR)中译码襟翼参数值。与神经网络模型的比较实践表明,该方法具有实用价值。     

基于反电势形状函数法的无刷直流电动机直接转矩控制

采用两相导通模式时通过逆变器开关状态不能确定电压空间矢量,现有方案是通过实时测量3个相电压来解决这一问题,但系统变得复杂;此外现有方案在转矩观测中包含的微分项会降低控制精度,增大计算量,影响系统实时性。针对这两点不足,提出反电势形状函数法,在软件中实现了相电压的实时计算,使转矩观测变得简洁,更易于工程实用。最后给出的仿真与实验结果证明了反电势形状函数法用于无刷直流电机直接转矩控制中的可行性与有效性。     

多随机变量的桁架结构系统的可靠性分析及优化设计

针对桁架结构系统，采用随机有限元法（SFEM）计算结构系统的响应量，考虑内力重新分配，建立失效模式的安全余量方程，用验算点法计算失效模式安全余量的可靠性指标，用改进的分枝限界法，寻找主要失效模式，通过对主要失效模式方程线性化研究，计算失效模式安全余量之间的相关系数，寻找主要失效模式，通过对主要失效模式方程线性化研究，计算失效模式安全余量之间的相关系数，最后用PNET法计算出结构系统的失效概率，同时给出多随机变量的结构系统可靠度的敏度表达式，采用最佳矢量法，求解了大型桁架结构系统基于可靠性指标约束下的最小重量的优化设计问题，最后，给出了实际算例，计算结果表明；采用随机有限元法能更好地考虑结构系统的多个随机变量对系统可靠性产生的影响；所采用的可靠性分析方法和优化方法是有效的。     

非线性逆在ASTOVL控制系统中的应用

研究了先进短距起飞垂直着陆飞机（ASTOVL）的飞行／推进控制系统的控制律，基于解和掌握气动舵面和推力矢量舵面控制下的飞机数学模型，应用非线性动态逆理论，为ASTOVL飞机从巡航到悬停阶段的飞行，设计了推力矢量控制器和俯仰控制器，以合理地分配飞机上的力和力矩，使得俯仰姿态速度和法向速度的控制在推进系统性能包括线范围内是近似线性和解耦的，最后以ASTOVL飞机悬停阶段的数字仿真曲线为例，证明了所设计的两个控制器是可行的，基本上达到了设计要求。     

太阳微波爆发精细结构与硬X射线耀斑的相关

北京天文台在２．８４ＧＨｚ频率上观测到的带短时标精细结构的微波爆发与日本ＹＯＨＫＯＨ卫星上ＨＸＴ在１９９１年１０月－１９９２年１２月观测到的硬Ｘ射线爆发（ＨＸＢ）事件作了比较，发现在２０个微波精细结构爆发事件只有１２个与ＹＯＨＫＯＨ卫星记录的ＨＸＢ有对应关系．本文对１９９２年６月７日典型事件中２．８４ＧＨｚ与ＨＸＢ共同存在的百秒量级的准周期振荡作了分析及源区参数的计算，并作了简要的讨论．