Hill区域内基于推广的Poincar映射的低能逃逸/捕捉轨道(英文)

给出了Hill区域内基于推广的Poincar映射的低能逃逸轨道的计算。文中的推广的Poincar映射需要在相空间中选取两个(而非一个)与流相截的面,即将包含某个天平动点的截面通过轨道来映射到近拱点的通道面上的,在数值上通过总变差减小的Runge-Kutta方法来实现两个相面之间的映射。捕捉轨道则可由Hill三体模型的对称性直接导出。最后,关于Rhea的二维、三维的逃逸和捕捉轨道的仿真结果验证了该方法的精度和鲁棒性。     

展向离散抽吸法控制边界层转捩实验研究

通过实验成功发展了一种生成大振幅稳定条带的有效方法,即展向离散抽吸方法。在此基础上,开展条带控制边界层转捩的研究。实验在水洞中进行,以零压力梯度平板边界层为研究对象,利用氢气泡时间线法观测引入条带前后人工激发转捩边界层中扰动发展变化,分析条带对转捩的控制效果及参数影响。结果表明,展向离散抽吸方法生成的稳定条带最大振幅可达28.4%U（U为自由流速度）;实验中引入的宽度14和28mm的稳定条带都能起到抑制转捩的作用;条带振幅越大、宽度越窄,抑制效果越明显。研究结果为探索降低水/空气中航行器摩阻的新技术提供有价值的参考。     

高超声速飞行器-进气道一体化热流数值计算

采用CFD(计算流体动力学)技术, 开展了飞行器前体/发动机一体化气动热环境分析.对层流区、转捩区和湍流区分别采用计算模型, 在湍流区利用压缩性修正的SSGZ-Jk-ε湍流模型, 在转捩区引入代数型转捩因子模型描述边界层由层流逐渐过渡为完全湍流的流动过程.计算了前体和内通道的表面热流, 并与实验结果进行了对比.结果表明所采用的计算方法可以较好地预测前体及发动机内通道热流率, 流动状态、几何结构及激波入射对热流值影响较大.      

PSE方法在后部加载叶栅绕流稳定性分析及转捩预测中的应用

采用数值求解与实验测量相结合的方法, 分析后加载叶栅绕流的稳定性并预测转捩.推导出正交曲线坐标系下三维扰动波的抛物化稳定性方程, 在风洞实验中测量叶栅叶片表面的静压分布, 并结合测量结果对设计叶栅的流动稳定性进行特征值分析.分析结果表明:(1)后加载叶型能有效推迟转捩, 提高叶栅的变冲角特性;(2)当冲角变化时叶顶流动稳定性的变化最显著, 负冲角流动稳定, 正冲角流动最不稳定.      

高超声速钝楔边界层转捩大涡模拟

 以五阶迎风和八阶对称格式混合差分格式求解三维可压缩滤波Navier-Stokes方程,对来流Mach数为6.0、半锥角5°的高超声速空间发展钝楔边界层转捩至完全湍流进行了大涡模拟。时间推进采用紧致存储三阶Runge-Kutta方法,亚格子尺度模型为Driest因子修正的Smagorinsky涡黏性模型。通过定常流场入口边界附近吹／吸引入不稳定扰动斜波的方法数值模拟得到了层流失稳转捩直至完全湍流的空间发展全过程。对扰动的线性、非线性增长以及湍流斑的形成和发展进行了分析,给出了转捩及完全湍流下的速度相关量统计并与实验、DNS结果进行了对比分析,计算结果与理论及实验吻合。     

月球着陆器精确定点及安全着陆技术研究

在未来月球探测中,需要对一些地形复杂的区域进行探测,而在这些区域软着陆,潜在的危险性增加,这就要求着陆时具有较高的定位精度并能够自动避险。当前,由于着陆时定点的误差较大,在小范围安全地域准确着陆很难。研究了一种精确定位、安全的软着陆方式,它在软着陆过程中增加了悬停阶段。在这一阶段中,通过着陆区危险地域的识别、着陆地点位置误差的计算,加上对着陆器横向漂移的控制技术,使着陆地点的精度以及着陆生存率大为提高,能够满足未来月球探测的软着陆要求。     

Longitudinal variation of the equatorial ionosphere: Modeling and experimental results

We describe a new version of the Parameterized Regional Ionospheric Model (PARIM) which has been modified to include the longitudinal dependences. This model has been reconstructed using multidimensional Fourier series. To validate PARIM results, the South America maps of critical frequencies for the E (foE) and F (foF2) regions were compared with the values calculated by Sheffield Plasmasphere-Ionosphere Model (SUPIM) and IRI representations. PARIM presents very good results, the general characteristics of both regions, mainly the presence of the equatorial ionization anomaly, were well reproduced for equinoctial conditions of solar minimum and maximum. The values of foF2 and hmF2 recorded over Jicamarca (12°S; 77°W; dip lat. 1°N; mag. declination 0.3°) and sites of the conjugate point equatorial experiment (COPEX) campaign Boa Vista (2.8°N; 60.7°W; dip lat. 11.4°; mag. declination −13.1°), Cachimbo (9.5°S; 54.8°W; dip lat. −1.8°; mag. declination −15.5°), and Campo Grande (20.4°S; 54.6°W; dip lat. −11.1°; mag. declination −14.0°) have been used in this work. foF2 calculated by PARIM show good agreement with the observations, except during morning over Boa Vista and midnight-morning over Campo Grande. Some discrepancies were also found for the F-region peak height (hmF2) near the geomagnetic equator during times of F₃ layer occurrences. IRI has underestimated both foF2 and hmF2 over equatorial and low latitude sectors during evening-nighttimes, except for Jicamarca where foF2 values were overestimated.     

拦截高速目标的比例与反比例导引捕获区分析

针对拦截高速目标的作战特点,分析了比例导引(PN)与反比例导引(RPN)的捕获区。首先,通过分析拦截弹与目标的相对运动关系,推导得到了顺轨和逆轨的零控拦截条件,此条件由目标和拦截弹的速度前置角以及二者速度比确定;其次,以拦截弹和目标速度前置角为坐标系,推导得到了PN以及RPN捕获区以及各自导航比设置范围。PN的捕获区由逆轨零控拦截条件以及与其相切且斜率为1/(N-1)的两条直线构成,RPN的捕获区由顺轨零控拦截条件以及与其相切且斜率为1/(-N-1)的两条直线构成;然后,利用函数对称性将PN与RPN捕获区转换到同一坐标区间,得到了相同条件下RPN捕获区要大于PN捕获区的结论;最后,开展了四种情形下的仿真,验证了本文捕获区分析的合理性及有效性。     

The Crab pulsar seen with AquEYE at Asiago Cima Ekar observatory

We are developing fast photon-counter instruments to study the rapid variability of astrophysical sources by time tagging photon arrival times with unprecedented accuracy, making use of a Rubidium clock and GPS receiver. The first realization of such optical photon-counters, dubbed AquEYE (the Asiago Quantum Eye), was mounted in 2008 at the 182 cm Copernicus Observatory in Asiago. AquEYE observed the Crab pulsar several times and collected data of extraordinary quality that allowed us to perform accurate optical timing of the Crab pulsar and to study the pulse shape stability on a timescale from days to years with an excellent definition. Our results reinforce the evidence for decadal stability of the inclination angle between the spin and magnetic axis of the Crab pulsar. Future realizations of our instrument will make use of the Galileo Global Navigation Satellite System (GNSS) time signal.     

Solar Sources of Heliospheric Energetic Electron Events—Shocks or Flares?

Electrons with near-relativistic (E≳30 keV, NrR) and relativistic (E≳0.3 MeV) energies are often observed as discrete events in the inner heliosphere following solar transient activity. Several acceleration mechanisms have been proposed for the production of those electrons. One candidate is acceleration at MHD shocks driven by coronal mass ejections (CMEs) with speeds ≳1000 km s⁻¹. Many NrR electron events are temporally associated only with flares while others are associated with flares as well as with CMEs or with radio type II shock waves. Since CME onsets and associated flares are roughly simultaneous, distinguishing the sources of electron events is a serious challenge. On a phenomenological basis two classes of solar electron events were known several decades ago, but recent observations have presented a more complex picture. We review early and recent observational results to deduce different electron event classes and their viable acceleration mechanisms, defined broadly as shocks versus flares. The NrR and relativistic electrons are treated separately. Topics covered are: solar electron injection delays from flare impulsive phases; comparisons of electron intensities and spectra with flares, CMEs and accompanying solar energetic proton (SEP) events; multiple spacecraft observations; two-phase electron events; coronal flares; shock-associated (SA) events; electron spectral invariance; and solar electron intensity size distributions. This evidence suggests that CME-driven shocks are statistically the dominant acceleration mechanism of relativistic events, but most NrR electron events result from flares. Determining the solar origin of a given NrR or relativistic electron event remains a difficult proposition, and suggestions for future work are given.