The Primordial Helium-4 Abundance from Observations of a Large Sample of Blue Compact Dwarf Galaxies

We use a sample of 45 low-metallicity H II regions in blue compact dwarf (BCD) galaxies to determine the primordial helium abundance YP with a precision better than 5%. We have carefully investigated the physical effects which may make the He I line intensities deviate from their recombination values such as collisional and fluorescent enhancements, underlying He I stellar absorption and absorption by Galactic interstellar Na I. By extrapolating the Y vs. O/H and Y vs. N/H linear regressions to O/H = N/H = 0, we obtain YP = 0.244±0.002 and 0.245±0.001, respectively, higher than previous determinations (YP = 0.230 - 0.234). Part of the difference comes from the fact that previous investigators have not taken into account underlying He I stellar absorption, especially in the NW component of the BCD I Zw 18 which, because of its extremely low metallicity plays a key role in the determination of YP. We derive a slope dY/dZ = 2.3±1.0, considerably smaller than those derived before. With this smaller slope and taking into account the errors, chemical evolution models with an outflow of well-mixed material can be built for star-forming dwarf galaxies which satisfy all the observational constraints. Our YP gives _bh ₅₀ ² = 0.058±0.007,f consistent with the lower limit set by dynamical measurements and X-ray observations of clusters of galaxies. It is also consistent, within the framework of standard big bang nucleosynthesis theory, with measurements of primordial 7Li in galactic halo stars and with the D/H abundance measured in absorption systems toward quasars by Burles and Tytler (1997).     

热流限制下的最优气动力辅助变轨

以变轨能量消耗最小为优化目标，应用极大值原理研究了飞行过程受热流限制和升力系统约束下的气动力辅助共面变轨问题，飞行过程成分第一自由弧段，约束弧段，第二自由弧段三个部分，讨论了升力系数的最优表达式，分析了飞行过程中两种约束的相互作用，给出了约束弧起始位置的角点条件和终端的横截条件下，对不同的初值选取方法讨论了三种计算策略，并给出了数值算例。     

航天器轨道追逃博弈多阶段强化学习训练方法

针对航天器轨道追逃博弈问题,提出一种多阶段学习训练赋能方法,使得追踪星在终端时刻抵近逃逸星的特定区域,而逃逸星需要通过轨道机动规避追踪星。首先,构建两星的训练策略集,基于逻辑规则设计追踪星和逃逸星的机动策略,通过实时预测对方的终端位置,设计己方的期望位置和脉冲策略,显式给出追逃策略的解析表达式,用于训练赋能;其次,为提升航天器的训练赋能效率及应对未知环境的博弈能力,提出一种基于强化学习技术多模式、分阶段的学习训练方法,先使追踪星和逃逸星分别应对上述逻辑规则引导下的逃逸星和追踪星,完成预训练;再次,开展二次训练,两星都采用邻近策略优化(PPO)策略进行追逃博弈,在博弈中不断调整网络权值,提升决策能力;最后,在仿真环境中验证提出的训练方法的有效性,经过二次训练后,追踪星和逃逸星可有效应对不同策略驱动下的对手,提升追逃成功率。     

结合损伤力学与有限元方法预估铆接结构疲劳寿命

利用飞机铆接试验件疲劳试验数据,结合损伤力学与有限元方法,通过MATLAB调用ABAQUS进行损伤演化方程参数的遗传优化反演。将反演得到的损伤演化方程用于飞机结构疲劳寿命预估中,对机翼蒙皮锪窝形式的铆接结构进行了寿命计算和分析,并与试验数据作对比,证明了方法的可行性。     

基于我国深空站三向测量模式的数据精度分析

为了验证我国深空站三向测量模式的正确性,以同步星跟踪试验中的测量数据为基础,建立了站间同步修正算法和三向测量观测模型,通过与同步卫星的精密星历反算测量值比较,得到了测量数据的标定参数,结果表明,我国深空站测控能够实现dm级的测量精度,明显优于“嫦娥二号”测量的水平;同时利用测量数据进行定轨策略分析,最终实现了10 m量级的同步卫星定轨精度.分析结果为“嫦娥三号”探测器实施有效测控提供了依据.     

基于损伤力学预估点蚀疲劳寿命有限元法

飞机使用环境谱的不断变化会对机体结构造成腐蚀损伤,工程上难以在外场环境下进行实时损伤检测与疲劳性能试验。点蚀作为腐蚀的初始阶段,危害性大,部位也难以预测。采用损伤力学和有限元相结合的方法,以材料疲劳S-N数据为基础,将点蚀损伤认为是一种初始缺陷,建立基于损伤力学假设的点蚀损伤疲劳寿命预估方法,并提出一种改进型损伤参数反演方法。对点蚀疲劳失效过程进行数值模拟,模拟结果与试验结果吻合,证明该方法应用于金属材料点蚀疲劳问题中是合理的、可行的,为后续实际预腐蚀损伤疲劳研究奠定了基础。     

微小推力下小卫星的轨道递推与推力标定

针对采用微小推力进行轨道机动的小卫星,考虑复杂摄动力的基础设计了一种高精度轨道外推和推力在轨标定算法.首先,建立了考虑地球复杂摄动力和微小推力的小卫星轨道动力学模型;然后基于动力学模型,利用变步长龙格库塔算法,设计了对微小推力小卫星进行高精度轨道外推的方法.随后通过无迹卡尔曼滤波器(UKF),设计在轨标定算法,对存在误...     

Diversity of Comets: Formation Zones and Dynamical Paths

The past dozen years have produced a new paradigm with regard to the source regions of comets in the early solar system. It is now widely recognized that the likely source of the Jupiter-family short-period comets (those with Tisserand parameters, T > 2 and periods, P, generally < 20 years) is the Kuiper belt in the ecliptic plane beyond Neptune. In contrast, the source of the Halley-type and long-period comets (those with T < 2 and P > 20 years) appears to be the Oort cloud. However, the comets in the Oort cloud almost certainly originated elsewhere, since accretion is very inefficient at such large heliocentric distances. New dynamical studies now suggest that the source of the Oort cloud comets is the entire giant planets region from Jupiter to Neptune, rather than primarily the Uranus-Neptune region, as previously thought. Some fraction of the Oort cloud population may even be asteroidal bodies formed inside the orbit of Jupiter. These comets and asteroids underwent a complex dynamical random walk among the giant planets before they were ejected to distant orbits in the Oort cloud, with possible interesting consequences for their thermal and collisional histories. Observational evidence for diversity in cometary compositions is limited, at best. This revised version was published online in June 2006 with corrections to the Cover Date.     

Dynamical evolution of high area-to-mass ratio debris released into GPS orbits

A large set of simulations, including all the relevant perturbations, was carried out to investigate the long-term dynamical evolution of fictitious high area-to-mass ratio (A/M) objects released, with a negligible velocity variation, in each of the six orbital planes used by Global Positioning System (GPS) satellites. As with similar objects discovered in near synchronous trajectories, long lifetime orbits, with mean motions of about 2 revolutions per day, were found possible for debris characterized by extremely high area-to-mass ratios. Often the lifetime exceeds 100 years up to A/M ∼ 45 m²/kg, decreasing rapidly to a few months above such a threshold. However, the details of the evolution, which are conditioned by the complex interplay of solar radiation pressure and geopotential plus luni-solar resonances, depend on the initial conditions. Different behaviors are thus possible. In any case, objects like those discovered in synchronous orbits, with A/M as high as 20–40 m²/kg, could also survive in this orbital regime, with semi-major axes close to the semi-synchronous values, with maximum eccentricities between 0.3 and 0.7, and with significant orbit pole precessions (faster and wider for increasing values of A/M), leading to inclinations between 30° and more than 90°.     

Neutron stars: Classification and evolution

The general aproach is considered which describs the evolution of neutron stars in terms of their interaction with surrounding matter. All possible states of neutron stars are classified from this point of view. Classification and evolution of binaries contaning neutron stars are also considered.