蓝色中性墨水的剖析

对蓝色中性墨水进行了系统分离 ,对分离组分进行了初步鉴定 ,确定了该墨水主要由溶剂水、颜料酞菁铜、非离子表面活性剂、保湿剂和增粘剂等组成 ,所测主要成分的质量分数为 99.7%。     

对直升机动力学的现状与发展的分析

对以旋翼动力学和飞行动力学为主体的直升机动力学研究进展回顾。主要讨论与飞行力学有关的旋翼气动力模型，旋翼结构动力学、气动弹性力学、飞行动力学模型与控制以及飞行操纵与品质等方面的进展，分析它们的现状，供有关直升机研究人员参考。     

The revised eccentric binary model for X Persei (4U 0352 + 30)

The eccentric binary model for X Persei is discussed with a view to most recent determination of mass, radius and mass loss rate. The existence of such a system depends critically on the value of viscosity in the outer layers of the star and, in the case where viscosity is induced by shear turbolence, on the axial rotational velocity. The parameters of the binary system are derived in the most favourable case.     

航空发动机火焰筒矩形点焊换段修理技术研究

针对某型航空发动机火焰筒大修时出现的裂纹、烧伤及侵蚀问题,开展了火焰筒第4～6段换段修理工艺试验。通过分析火焰筒的结构,确定了用新段替换相应的故障段的方法对火焰筒进行修复。在拆分故障段时,尽量减小保留段壁厚的局部减薄量;在重新装配时,避免在原电阻焊点处再次焊接;通过采取以上工艺措施,实现了火焰筒的换段修理。同时进行了电阻焊焊接拉伸试验、撕破检查、金相组织检查等工艺验证试验。换段修理的火焰筒通过了发动机试车考核验证。换段工艺方法也可作为批生产过程中部分段制造有缺陷时的补救方案。     

Collisional profiles of ionized calcium perturbed by helium

The spectra of many cool DZ white dwarfs show extremely broad resonance lines of ionized calcium and magnesium in the optical and ultraviolet region. When the line center is strongly saturated, these wings may become a significant source of additional opacity in cool white dwarf atmospheres. The omission of this opacity results in systematic errors in the predicted flux distribution and hence in the effective temperatures and element abundances. In a continuation of Homeier et al. (2007) and Allard et al. (2012), where we presented absorption spectra of Na–He in cool white dwarfs, we extend this work to the Ca⁺–He system.     

LiHe spectra from brown dwarfs to helium clusters

The detection of Li I lines is the most decisive spectral indicator of substellarity for young brown dwarfs with masses below about 0.06 solar mass. Due to the weakness of the Li resonance lines, it is important to be able to model precisely both their core widths and their wing profiles. This allows an adequate prediction of the mass at which Li lines reappear in the spectra of brown dwarfs for a given age, or reversely an accurate determination of the age of a cluster. We report improved line profiles and the dependence of line width on temperature suitable for modeling substellar atmospheres that were determined from new LiHe molecular potential energies. Over a limited range of density and temperature, comparison with laboratory measurements was used to validate the potential energies which support the spectral line profile theory.     

Evolution of the temporal and the spectral properties in 2010 and 2011 outbursts of H 1743-322

The Galactic black hole candidate H 1743-322 exhibited two X-ray outbursts in rapid succession: one in August 2010 and the other in April 2011. We analyze archival data of this object from the PCA instrument on board RXTE (2–25 keV energy band) to study the evolution of its temporal and spectral characteristics during both the outbursts, and hence to understand the behavioral change of the accretion flow dynamics associated with the evolution of the various X-ray features. We study the evolution of QPO frequencies during the rising and the declining phases of both the outbursts. We successfully fit the variation of QPO frequency using the Propagating Oscillatory Shock (POS) model in each of the outbursts and obtain the accretion flow parameters such as the instantaneous shock locations, the shock velocity and the shock strength. Based on the degree of importance of the thermal (disk black body) and the non-thermal (power-law) components of the spectral fit and properties of the QPO (if present), the entire profiles of the 2010 and 2011 outbursts are subdivided into four different spectral states: hard, hard-intermediate, soft-intermediate and soft. We attempt to explain the nature of the outburst profile (i.e., hardness-intensity diagram) with two different types of mass accretion flow.     

Feature selection for high-dimensional data in astronomy

With an exponentially increasing amount of astronomical data, the complexity and dimension of astronomical data are likewise growing rapidly. Extracting information from such data becomes a critical and challenging problem. For example, some algorithms can only be employed in the low-dimensional spaces, so feature selection and feature extraction become important topics. Here we describe the difference between feature selection and feature extraction methods, and introduce the taxonomy of feature selection methods as well as the characteristics of each method. We present a case study comparing the performance and computational cost of different feature selection methods. For the filter method, ReliefF and fisher filter are adopted; for the wrapper method, improved CHAID, linear discriminant analysis (LDA), Naive Bayes (NB) and C4.5 are taken as learners. Applied on the sample, the result indicates that from the viewpoints of computational cost the filter method is superior to the wrapper method. Moreover, different learning algorithms combined with appropriate feature selection methods may arrive at better performance.     

Numerical Simulations of the Warm-Hot Intergalactic Medium

In this paper we review the current predictions of numerical simulations for the origin and observability of the warm hot intergalactic medium (WHIM), the diffuse gas that contains up to 50 per cent of the baryons at z∼0. During structure formation, gravitational accretion shocks emerging from collapsing regions gradually heat the intergalactic medium (IGM) to temperatures in the range T∼10⁵–10⁷ K. The WHIM is predicted to radiate most of its energy in the ultraviolet (UV) and X-ray bands and to contribute a significant fraction of the soft X-ray background emission. While O vi and C iv absorption systems arising in the cooler fraction of the WHIM with T∼10⁵–10^5.5 K are seen in FUSE and Hubble Space Telescope observations, models agree that current X-ray telescopes such as Chandra and XMM-Newton do not have enough sensitivity to detect the hotter WHIM. However, future missions such as Constellation-X and XEUS might be able to detect both emission lines and absorption systems from highly ionised atoms such as O vii, O viii and Fe xvii.     

Thermal Radiation Processes

We discuss the different physical processes that are important to understand the thermal X-ray emission and absorption spectra of the diffuse gas in clusters of galaxies and the warm-hot intergalactic medium. The ionisation balance, line and continuum emission and absorption properties are reviewed and several practical examples are given that illustrate the most important diagnostic features in the X-ray spectra.