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欧洲核子研究中心的大型强子对撞机近日在底夸克实验中发现了两种新型粒子——DS3＊和DS1＊DS3＊的自旋为3。这是首次观察到的包含一个粲夸克的自旋为3的粒子。在其他介子中，夸克可以以几种不同方式中的一种成形．使得粒子的自旋不到3，并使夸克的确切性质变得模糊不清。自旋达到3的粒子就不存在这种含糊状态，所以DS3＊的确切构造很清晰。     

余辉等离子体的实验研究

利用调制脉冲产生的余辉等离子体的参数测量表明:等离子体空间电位和电子温度的衰变是重要的,它在余辉等离子体的密度衰变过程研究中必须予以考虑.对容器中余辉等离子体密度径向分布的测量结果与理论预言是一致的.     

2D and 3D MHD simulations of disk accretion by rotating magnetized stars: Search for variability

We performed 2D and full 3D magnetohydrodynamic simulations of disk accretion to a rotating star with an aligned or misaligned dipole magnetic field. We investigated the rotational equilibrium state and derived from simulations the ratio between two main frequencies: the spin frequency of the star and the orbital frequency at the inner radius of the disk. In 3D simulations we observed different features related to the non-axisymmetry of the magnetospheric flow. These features may be responsible for high-frequency quasi-periodic oscillations (QPOs). Variability at much lower frequencies may be connected with restructuring of the magnetic flux threading the inner regions of the disk. Such variability is specifically strong at the propeller stage of evolution.     

Numerical simulation of three-dimensional reconnection due to the instability of collisionless current sheets

Based on analytical calculations we have currently argued that spontaneous reconnection through thin collisionless current sheets is an essentially three-dimensional (3 D) process (Büchner, 1996 a, b). Since 3 D kinetic PIC codes have become available, the three dimensional nature of the collisionless current sheet decay are now illustrated by numerical simulations (Büchner and Kuska, 1996; Pritchett and Coroniti, 1996; Zhu and Winglee, 1996). While the latter two claim a coupling to a longer wavelength kink mode as a main factor, destabilizing thin current sheets in 3 D, our simulations have revealed that even shorter scale perturbations in the current direction suffice to destabilize thin sheets very quickly. Since past simulation runs, however, were limited to mass ratios near unity, the influence of the electrons was not treated adequately. We have now investigated the stability of thin collisionless current sheets including 64 times lighter negatively charged particles. We can now show that while the two-dimensional tearing instability slows down for M = M_p/m_e = 64, the three-dimensional current sheet decay is a much faster process — practically as fast as the mass ratio M = 1 3 D sheet decay, even without kinking the sheet. We further conclude that, unlike the two-dimensional tearing instability, the three-dimensional decay of thin current sheets is not controlled by the electrons. For a sheet width comparable with the ion inertial length, we also recovered signatures of the Hall effect as predicted by Vasyliunas (1975) in the mass ratio M = 64 case. The ion inertial length seems to be the critical scale at which the sheet starts to decay.     

Analysis of GNSS clock prediction performance with different interrupt intervals and application to real-time kinematic precise point positioning

Continuous and timely real-time satellite orbit and clock products are mandatory for real-time precise point positioning (RT-PPP). Real-time high-precision satellite orbit and clock products should be predicted within a short time in case of communication delay or connection breakdown in practical applications. For prediction, historical data describing the characteristics of the real-time orbit and clock can be used as the basis for performing the prediction. When historical data are scarce, it is difficult for many existing models to perform precise predictions. In this paper, a linear regression model is used to predict clock products. Seven-day GeoForschungsZentrum (GFZ) final clock products sampled at 30 s are used to analyze the characteristics of GNSS clocks. It is shown that the linear regression model can be used as the prediction model for the satellite clock products. In addition, the accuracy of the clock prediction for different satellites are analyzed using historical data with different periods (such as 2 and 10 epochs). Experimental results show that the accuracy of the clock with the linear regression prediction model using historical data with 10 epochs is 1.0 ns within 900 s. This is higher accuracy than that achieved using historical data of 2 epochs. Finally, the performance analysis for real-time kinematic precise point positioning (PPP) is provided using GFZ final clock prediction results and state space representation (SSR) clock prediction results when communication delay or connection breakdown occur. Experimental results show that the positioning accuracy without prediction is better than that with prediction in general, whether using the final clock product or the SSR clock product. For the final clock product, the positioning accuracy in the north (N), east (E), and up (U) directions is better than 10.0 cm with all visible GNSS satellites with prediction. In comparison, the 3D positioning accuracy of N, E, and U directions with visible GNSS satellites whose prediction accuracy is better than 0.1 ns using historical data of 10 epochs is improved from 15.0 cm to 7.0 cm. For the SSR clock product, the positioning accuracy of N, E, and U directions is better than 12.0 cm with visible GNSS satellites with prediction. In comparison, the 3D positioning accuracy of N, E, and U directions with visible GNSS satellites whose prediction accuracy is better than 0.1 ns using historical data of 10 epochs is improved from 12.0 cm to 9.0 cm.     

软件可靠性预计方法研究及实现

软件可靠性评估可以估计和预计软件可靠性水平.为了解决软件可靠性预计过程中存在的问题,提出了一种软件可靠性预计方法.该方法通过分析和改进模型的预计质量来选择模型进行预计,对模型预计质量的分析使用了U图、Y图和对数PLR图,再标定法和组合法被用于改进模型的预计质量.在该方法的基础上开发了软件可靠性分析工具,此工具可以进行多种软件可靠性模型的原始预计、预计质量分析和改进原始模型的预计质量.     

适于旋流杯下游流场的改进型半分析关系式

利用典型(CFM-56燃烧室)旋流杯结构下游的流场实验数据,参照经验关系式,提出了物理意义更明确、拟合更准确、且更便于对大量实验数据进行相关性研究的半经验关系式,并与旋流杯下游紧靠出口处附近的轴向速度及旋流速度测量数据进行了对比,发现各特征数据(如峰值位置、峰值衰减速度、回流区宽度及其沿下游的发展、回流速度及其衰减等)与实验数据非常相符,从而初步验证了提出的半经验关系式.同时,给出了公式中不同的经验常数取值带来的变化,分析了与几何及工况参数之间可能的联系,为进一步验证该关系式打下基础.分析表明,各经验常数的变化之间相互独立,且物理意义明确,可以方便地用于进一步验证.      

基于轨道预报的热层模式评估

在太阳活动高低年的地磁平静/扰动环境下,利用不同热层大气模式J77,DTM78,MSIS00,JB2008和CHAMP加速度计反演密度,分析有无先验信息条件下的轨道预报误差.结果表明无先验信息的精密轨道预报中,热层模式的性能可能被弹道系数等参数偏差干扰,此时预报误差不能作为模式性能的评价标准.先验信息对轨道预报精度提升非常明显,尤其是地磁扰动期先进热层模式性能得以展现,轨道预报误差为无先验信息情况下的10%～25%.目前热层模式的主要缺陷存在于地磁扰动期.各模式之间的差异是:JB2008模式可以通过线性和单一频率周期项补偿,而J77及DTM78等模式还存在更多频率的误差.本文对不同情况下精密轨道预报的研究结果可为空间碎片碰撞预警等工程实践提供参考.      

含孔隙基体缎纹编织复合材料面内压缩弹性性能预报

缎纹编织复合材料细观结构复杂,传统弹性性能预报方法较难适用。针对该问题,建立缎纹编织复合材料代表体积单元(RVE),对RVE模型面内压缩弹性模量和面内泊松比的预报方法进行了研究。分别基于能量法原理和单夹杂理论,对弯曲纤维束纵向压缩模量和含孔隙基体弹性性能进行预报,改进了传统细观力学中的混合率方法,并利用已得的组分材料性能对RVE模型有效面内压缩模量和面内泊松比实现了解析法预报。基于Python语言对ABAQUS有限元分析软件进行二次开发,建立了基体含孔隙的RVE模型,利用RVE模型在基本受力状态下的有限元方法结果实现有效面内压缩模量和面内泊松比的有限元方法预报。基于碳/碳复合材料,解析法与数值法计算结果吻合很好,实现了对缎纹编织材料面内压缩性能的有效预报。      

复合材料结构三维有限元分析的材料参数

在调研现有文献复合材料结构三维数值分析中材料参数的基础上,阐述了基于单层板材料性能数据建立复合材料三维材料参数的方法.通过对复合材料π接头结构的三维数值模拟和试验,研究了三维材料参数中不确定参数对结构刚度预测的影响;分别采用三维修正的最大应力准则、最大应变准则、蔡-胡准则和Hashin准则评价π接头的初始破坏,结合试验数据,研究不同失效准则对复合材料π接头结构的适用范围以及材料参数对初始破坏强度预测的影响.研究工作可为一般层合复合材料结构的三维建模提供参考,并为深入理解复合材料π接头结构力学性能、准确预测其破坏强度提供理论支持.     

Simulation software for the spiral trajectory of our Moon

At 4.56 Ga, the accretion of the slowly rotating Solar Nebula led to the formation of Sun and its Planets in the plane of disc of accretion. Moon was formed by accretion from a circumterrestrial disk of debris generated by the glancing angle impact of the young Earth by a Mars size planetary embryo at about 4.5 Ga at a distance of 15,000 km. The Moon since then has migrated to the present position of 384,400 km from the center of the Earth. In course of this outward migration it has slowed down the spin rate of Earth and caused the lengthening of diurnal day length from 5 h initially to 24 h presently. The basic mechanics of Earth–Moon System has been worked out and theoretical determination of lengthening of day curve is carried out. This theoretical lengthening of day curve is compared with the observed lengthening of day curve based on paleobotanical evidences, ancient tidalites and Australian Banded Iron Formation. There is a remarkable correspondence between the two curves except for intermittent deviations due to geographical and geophysical factors. Based on the theoretical curve of lengthening of day, an empirical formula for the lunar orbital radius expansion is determined. Based on this empirical formula, simulation software is developed that gives the correct evolution of the semi-major axis (a) of our Moon for any time span from the inception to the time chosen under study. For mathematical simplicity the system is considered to be a two body rotating system throughout its evolutionary history of 4.5 Gyrs. This simulation draws the Moon’s spiral trajectory from its inception to any subsequent epoch. The terminal epoch is an input to the simulation software to arrive at the spiral trajectory of the Moon from the inception to the given epoch. The basic mechanics of Earth–Moon System and this simulation can be generalized to lay the foundation of simulation software for any Planet–Satellite pair or any Sun-Planet pair in our Solar System or Star-Planet pair in any Extra-Solar System. The basic dynamics has been found to be valid for Star–Planet pair also. So this Simulation Methodology can as well be applied to study the migratory evolution of Gas Giants also.