考虑轨道摄动的外热流计算分析

为改进传统外热流算法未考虑外热流经多次反射后的吸收和国外商业软件未考虑轨道摄动及太阳矢量变化对外热流的影响等不足,重新定义了外热流角系数和外热流辐射传递因子,综合SGP4轨道模型和Gebhart方法,给出了考虑摄动等因素的辐射传递因子和轨道外热流计算模型,以及相应的计算流程。通过仿真分析论证了考虑多次反射及摄动等因素的重要性。     

建构主义教学模式对大学生学习方式影响研究

建构主义教学模式对大学生学习方式有重要影响,通过实证研究方法,研究了课堂环境下建构主义教学模式与大学生学习方式之间的内在关系。研究结果表明：以互动性、自主性为特征的建构主义教学模式与深层学习方式显著正相关,教学模式中的自主性对深层动机和策略的影响均显著高于互动性,且自主性可以更为有效地促使学生采用深层学习方式。     

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。     

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°.     

Stellar winds of massive stars in M31

We have obtained the first UV high resolution spectra of hot luminous stars in M31 with the FOS onHubble Space Telescope. The spectra, combined with optical spectroscopic and photometric observations, enable us to study their stellar winds and photospheric parameters. We derive mass-loss rates and velocity laws from the wind line profiles, with the SEI method, as well as information on abundances. The wind lines and photospheric spectra are compared with galactic stars of the same spectral type.The spectra analyzed so far indicate that the stars have mass-loss rates comparable or slightly lower than galactic stars of the same spectral type, but possibly different velocity laws in their winds. The spectra of two stars are discussed here.     

Keck observations of ROSAT ultra-luminous X-ray source candidates

We present results of optical follow-up observations of candidate ultra-luminous X-ray sources (ULXs). Using Keck optical spectroscopy, 17 of the candidates from the Colbert and Ptak [Colbert, E.J.M., Ptak, A.F. A catalog of candidate intermediate-luminosity X-ray objects. ApJS 143, 25–45, 2002] catalog have been identified; this is one of the largest sets of optical identifications of such objects thus far. Fifteen are background active galactic nuclei (AGN); two are foreground stars in our Galaxy. These findings are consistent with background and foreground object expectations, as derived from log N–log S relations. Also, the results are briefly discussed in terms of the spiral-galaxy/ULX connection.     

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.     

On kinematics of gas clouds in the broad-line region of active galactic nuclei and quasars

The kinematics of gas clouds in broad-line region of active galactic nuclei and quasars is considered. The motion of the clouds is governed by three forces — gravitational influence from the central supermassive body, radiational pressure from the continuum radiation, and resistance of the intercloud medium. Clouds moves radial but only outward motion gives a velocity field, which is in accordance with the observational data. The profiles of the permited lines are obtained in some simplify assumptions for the emissive capacity of the gas in clouds, and are in good agreement with the observational data. In the framework of the model under consideration there is a possibility to estimate some physical parameters of the nuclei such as mass of the central body and density of the intercloud medium.