Relativistic proton production at the Sun in the 20 January 2005 solar event

Based on the concept of multiple acceleration of solar energetic particles (SEP) we analyzed the super-event of 20 January 2005 by the data of ground level, balloon and spacecraft observations. The main characteristics of relativistic solar protons (energy spectra, anisotropy directions and pitch-angle distributions) are derived and their dynamics during the event is studied. It is shown that the flux of relativistic solar protons may consist of two distinct components, the so-called prompt and delayed ones. Within a two-source model of particle generation, one of which is associated with an expanding magnetic loop, we solved the transport equation in energy phase space, including adiabatic losses simultaneously with the stochastic acceleration process, and calculate the expected spectra of the delayed component at the source. The confrontation of experimental spectra with theoretical ones shows that the delayed component may be correctly described by stochastic acceleration, but not the prompt component. The required acceleration efficiencies turned out to be rather high, so that, for this particular event, adiabatic cooling is practically negligible. Our results provide a new support to the existence of two populations of relativistic solar protons in some SEP events.     

非圆截面弹体附加表面积工程估算方法研究

引入附加质量、附加表面积的概念 ,给出基于细长体理论的非圆截面弹体附加表面积的工程估算方法 ,并提出了计算带倒角圆的正方形和不同顶角菱形附加表面积的通用公式 ,通过计算值与理论值的比较 ,误差在 2 %以内。并通过利用附加表面积计算的弹体法向力系数与试验值进行比较 ,法向力系数计算误差在 10 %以内 ,说明用本方法计算的附加表面积可以在工程初步估算时应用。     

空间站微重力环境研究与分析

太空中的微重力环境对基础科学研究和新技术开发具有重要意义,为了满足未来我国空间站开展微重力科学实验的需求,需要对空间站上的微重力水平进行分析和评估,指导高微重力要求实验载荷的布局和微重力实验期间的飞行任务规划。空间站上的微重力水平用加速度值度量,通常可以分为准稳态加速度、瞬态加速度和振动加速度。针对此问题调研总结了国际空间站的微重力研究情况,并以400 km轨道高度上100吨级"T"字型积木式空间站作为算例,估算其准稳态加速度大小及分布,并初步分析瞬态加速度水平的量级。结果表明,空间站准稳态加速度水平在1μgn量级,主要贡献来自重力梯度效应;瞬态加速度可达103μgn量级。文章对将来我国空间站微重力应用支持的设计工作有一定的借鉴意义。     

长时间小过载条件下发动机流场特征及绝热层烧蚀分析

以揭示固体火箭发动机在飞行条件下绝热层的异常烧蚀特性为目的,针对小过载、长作用时间条件下大长径比流道的发动机开展了三维两相流场的数值模拟研究,详细分析了发动机内流道内不同区域的颗粒聚集特征,并结合发动机失效部位处绝热层的烧蚀形貌进行了失效模式分析,针对性地提出了改进措施.研究结果表明:(1)不同过载条件下发动机内颗粒聚集和分布状态受过载大小和发动机流道结构共同作用且影响规律复杂,所引起的绝热层异常烧蚀模式和机理不同,特别是小过载长作用时间条件下的异常烧蚀需要引起设计者重视.(2)颗粒聚集在绝热层表面的换热或冲蚀都将引起绝热层局部烧蚀加剧,形成的“凹坑或凹槽”烧蚀形貌会造成颗粒的二次聚集效应,进而加剧烧蚀过程.(3)通过增加发动机旋转动作和局部绝热层加厚,可以提高发动机的飞行安全性.     

基于预测模型迭代优化的改进比例导引律

为了提高对加速度时变机动目标的制导精度,将预测决策理论与传统比例导引(PN)相结合,提出了一种通过泰勒级数预测模型迭代控制加速度修正项的改进比例导引律。首先,以预设的低阶泰勒级数预测模型预测特定时间的位移,并计算位移预测值与测量值的差值;然后,通过迭代方法逐阶增加泰勒级数预测模型阶数,直至满足精度要求;最后,计算泰勒级数预测模型的二阶导数,修正比例导引律的加速度指令。仿真结果表明,传统PN和APN的脱靶量分别约为195 m和95 m,提出的改进比例导引律的脱靶量约为8.3 m,极大地提高了制导精度。     

定时截尾数据回归分析方法

提出定时截尾数据回归分析方法,建立定时截尾数据回归方程,给出回归系数和标准差的最佳无偏整体估计、百分位值的点估计及其置信限估计.详细讨论了工程中常见的极值分布、Weibull分布、正态分布以及一般位置-尺度分布场合下定时截尾数据的回归分析问题.该方法可以充分利用截尾时刻的试验信息,并将各个状态下的定时截尾数据作为一个整体进行统计分析,具有信息量大、精度高的特点,从而可以在试验时间、经费等有限的情况下对产品进行高精度的寿命预测和可靠性评估.     

Constructing G~2 Continuous Curve on Freeform Surface with Normal Projection

This article presents a new method for G～2 continuous interpolation of an arbitrary sequence of points on an implicit or parametric surface with prescribed tangent direction and curvature vector,respectively,at every point.First,a G～2 continuous curve is constructed in three-dimensional space.Then the curve is projected normally onto the given surface.The desired interpolation curve is just the projection curve,which can be obtained by numerically solving the initialvalue problems for a system of first-order ordinary differential equations in the parametric domain for parametric case or in three-dimensional space for implicit case.Several shape parameters are introduced into the resulting curve,which can be used in subsequent interactive modification so that the shape of the resulting curve meets our demand.The presented method is independent of the geometry and parameterization of the base surface.Numerical experiments demonstrate that it is effective and potentially useful in numerical control (NC) machining,path planning for robotic fibre placement,patterns design on surface and other industrial and research fields.     

正弦力校准中质量块加速度分布影响的理论修正研究

通过理论分析得到质量块加速度分布影响的理论修正公式,并利用有限元法验证了理论公式,同时对实际应用中理论公式的修正偏差作出估计,为动态力校准的不确定度分析提供了可靠依据。     

Heating heavy ions in the polar corona by collisionless shocks: A one-dimensional simulation

Recently a new model for explaining the observations of preferential heating of heavy ions in the polar solar corona was proposed ( and ). In that model the ion energization mechanism is the ion reflection off supercritical quasi-perpendicular collisionless shocks in the corona and the subsequent acceleration by the motional electric field E = −V × B/c. The mechanism of heavy ion reflection is based on ion gyration in the magnetic overshoot of the shock. The acceleration due to the motional electric field is perpendicular to the magnetic field, giving rise to large temperature anisotropy with T_⊥ ? T_∥, in agreement with SoHO observations. Such a model is tested here by means of a one dimensional test particle simulation where ions are launched toward electric and magnetic profiles representing the shock transition. We study the dynamics of O⁵⁺, as representative of coronal heavy ions for Alfvénic Mach numbers of 2–4, as appropriate to solar corona. It is found that O⁵⁺ ions are easily reflected and gain more than mass proportional energy with respect to protons.     

Particle acceleration and gamma rays in solar flares: Recent observations and new modeling

Experiments on SMM, GAMMA, Yohkoh, GRANAT, Compton GRO, INTEGRAL, RHESSI and CORONAS-F satellites over the past three decades have provided copious data for fundamental research relating to particle acceleration, transport and energetics of flares and to the ambient abundance of the solar corona, chromosphere and photosphere. We summarize main results of solar gamma-astronomy (including some results of several joint Russian–Chinese projects) and try to appraise critically a real contribution of those results into modern understanding of solar flares, particle acceleration at the Sun and some properties of the solar atmosphere. Recent findings based on the RHESSI, INTEGRAL and CORONAS-F measurements (source locations, spectrum peculiarities, ³He abundance etc.) are especially discussed. Some unusual features of extreme solar events (e.g., 28 October 2003 and 20 January 2005) have been found in gamma-ray production and generation of relativistic particles (solar cosmic rays, or SCR). A number of different plausible assumptions are considered concerning the details of underlying physical processes during large flares: (1) existence of a steeper distribution of surrounding medium density as compared to a standard astrophysical model (HSRA) for the solar atmosphere; (2) enhanced content of the ³He isotope; (3) formation of magnetic trap with specific properties; (4) prevailing non-uniform (e.g., fan-like) velocity (angular) distributions of secondary neutrons, etc. It is emphasized that real progress in this field may be achieved only by combination of gamma-ray data in different energy ranges with multi-wave and energetic particle observations during the same event. We especially note several promising lines for the further studies: (1) resonant acceleration of the ³He ions in the corona; (2) timing of the flare evolution by gamma-ray fluxes in energy range above 90 MeV; (3) separation of gamma-ray fluxes from different sources at/near the Sun (e.g., different acceleration sources/episodes during the same flare, contribution of energetic particles accelerated by the CME-driven shocks etc.); (4) asymmetric magnetic geometry and new magnetic topology models of the near-limb flares; (5) modeling of self-consistent time scenario of the event.