Solar neutron events as a tool to study particle acceleration at the Sun

The Sun provides unique opportunities to study particle acceleration mechanisms using data from detectors placed on the Earth’s surface and on board spacecrafts. Particles may gain high energies by several physical mechanisms. Differentiating between these possibilities is a fundamental problem of cosmic ray physics. Energetic neutrons provide us with information that keeps the signatures of the acceleration site. A summary of some representative solar neutron events observed on the Earth’s surface, including associated X and γ-ray observations from spacecrafts is presented. We discuss evidence of acceleration of particles by the Sun to energies up to several tens of GeV. In addition, a recent solar neutron event that occurred on September 7th 2005 and detected by several observatories at Earth is analyzed in detail.     

Solar Energetic Particle Composition, Energy Spectra, and Space Weather

Recent progress in measuring the composition and energy spectra of solar energetic particles (SEPs) accelerated by CME-driven shocks is reviewed, including a comparison of the observed charge-to-mass dependence of breaks in SEP spectra with model predictions. Also discussed is a comparison of SEP and CME kinetic energies in seventeen large SEP events, and estimates of the SEP radiation dose that astronauts would be subject to once they venture outside the protective cover of Earth’s magnetosphere.     

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.     

考虑地面效应的翼型动态特性数值模拟

为了研究考虑地面干扰的飞行器非定常气动特性,基于滑移网格技术,通过求解二维非定常Euler方程,对不同近地高度下的NACA0012翼型的动态振动特性进行了数值模拟。分析了存在地面干扰时的升力系数以及俯仰力矩系数迟滞环变化,并结合强迫振动法,计算了翼型各个近地高度下的纵向组合动导数。结果表明,地面效应不仅对定常流场产生影响,更显著地影响了非定常气动力及力矩,近地高度越小,这种效应越明显,使得升力系数的迟滞环面积变小,幅值减小,而俯仰力矩系数的迟滞环变化不规律,力矩系数的动导数随着近地高度减小而增大(绝对值减小),纵向的动态稳定性产生损失。地面效应干扰在飞行器非定常气动研究中应该引起重视。     

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.     

A new online modelling method for aircraft engine state space model

To overcome the drawbacks of current modelling method for aircraft engine state space model, a new method is introduced. The form of state space model is derived by using Talyor series to expand the nonlinear model that is implicit equations and involves many iterations. A partial derivative calculation method for iterations is developed to handle the influence of iterations on parameters. The derivative calculation and the aerothermodynamics calculations are combined in the component level model with fixed number Newton-Raphson (N-R) iterations. Mathematical derivation and simulations show the convergence ability of proposed method. Simulations show that comparing with the linear parameter varying model and centered difference based state space model, much higher accuracy of proposed online modelling method is achieved. The accuracy of the state space model built by proposed method can be maintained when the step amplitudes of inputs are within 2%, and the responses of the state space model can match those of the component level model when each input steps larger amplitudes. In addition, an online verification was carried out to show the capability of modelling at any operating point and that state space model can predict future outputs accurately. Thus, the effectiveness of the proposed method is demonstrated.     

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。     

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.