美术与感觉寻求的关系

阐述了感觉寻求研究中与绘画有关的研究,分析感觉寻求人格与绘画的复杂度、风格倾向、内容的积极性以及艺术的不确定性之间的关系,认为美术学习可能会影响到人格的发展趋势,影响其创造性人格特质的形成。     

Purification and characterization of an alkaline protease from Acetes chinensis

An alkaline protease from Acetes chinensis was purified and characterized in this study. The steps of purification include ammonium sulfate precipitation, ion-exchange chromatography with Q-sepharose Fast Flow, gel filtration chromatography with S300 and the second ion-exchange chromatography with Q-sepharose Fast Flow. The protease was isolated and purified, which was present and active on protein substrates (azocasein and casein). The specific protease activity was 17.15 folds and the recovery was 4.67. The molecular weight of the protease was estimated at 23.2 kD by SDS-PAGE. With azocasein as the susbstrate, the optimal temperature was 55°C and the optimal pH value was 5.5. Ion Ca²⁺ could enhance the proteolytic activity of the protease, while Cu²⁺, EDTA and PMSF could inhibit its activity.     

EVOLUTION OF RAPIDS OF CREEK MOUTH－BAR AT GEZHOUBA RESERVOIR AND THE IMPACTS ON NAVIGABLE CHANNEL IN THE UPPER REACHES OF THE CHANGJIANG RIVER

ＥＶＯＬＵＴＩＯＮＯＦＲＡＰＩＤＳＯＦＣＲＥＥＫＭＯＵＴＨ－ＢＡＲＡＴＧＥＺＨＯＵＢＡＲＥＳＥＲＶＯＩＲＡＮＤＴＨＥＩＭＰＡＣＴＳＯＮＮＡＶＩＧＡＢＬＥＣＨＡＮＮＥＬＩＮＴＨＥＵＰＰＥＲＲＥＡＣＨＥＳＯＦＴＨＥＣＨＡＮＧＪＩＡＮＧＲＩＶＥＲ￥ＬｉｎＣ...     

地月系L_2点中继星激光测距成功率的估算

为了模拟位于地月系L2点的中继星"鹊桥"与月球的位置关系,进而估算中继星激光测距的成功率,按照轨道周期约为14天的要求对中继星所在的晕轨道进行计算,建立了一个综合考虑望远镜抖动、大气抖动和预报轨道横向偏离的模型。从数值上给出了一条轨道周期为14. 78天,X方向(地月连线方向)振幅为12 493 km,Y方向为34 596 km,Z方向(垂直于地月轨道平面方向)为11 916 km的周期轨道。由于晕轨道的最小振幅远大于月球遮挡的临界振幅4 000 km,因此月球对中继星不存在遮挡问题。基于建立的测距成功率模型,根据昆明站(国际编号:7820)的激光测距系统对运行在该轨道上的中继星进行测距成功率分析,结果表明:测距成功率随着中继星横向轨道标准差的增大呈快速降低的趋势。对于中继星到测站的平均距离而言,当中继星没有横向偏离时,探测器产生的光电子数为0. 151,成功率为14. 07%;横向偏离2 km时,光电子数降为0. 035,成功率降为3. 46%。对比最近距离与最远距离的情况,无横向偏离的情况下,探测器产生的光电子数从0. 174降为0. 139,成功率从16. 01%降为13. 02%。该计算结果可为云南天文台1. 2 m望远镜实现中继星激光测距提供参考。     

Voids in a ΛCDM universe

We study the formation and evolution of voids in the dark matter distribution using various simulations of the popular Λ cold dark matter cosmogony. We identify voids by requiring them to be regions of space with a mean overdensity of −0.8 or less – roughly the equivalent of using a spherical overdensity group finder for haloes. Each of the simulations contains thousands of voids. The distribution of void sizes in the different simulations shows good agreement when differences in particle and grid resolution are accounted for. Voids very clearly correspond to minima in the smoothed initial density field. Apart from a very weak dependence on the mass resolution, the rescaled mass profiles of voids in the different simulations agree remarkably well. We find a universal void mass profile of the form  ρ(< r )/ρ( r _eff) ∝ exp[( r / r _eff)^α]  , where r _eff is the effective radius of a void and  α∼ 2  . The mass function of haloes in voids is steeper than that of haloes that populate denser regions. In addition, the abundances of void haloes seem to evolve somewhat more strongly between redshifts ∼1 and 0 than the global abundances of haloes.     

A new lunar absolute control point: established by images from the landing camera on Chang'e-3

The establishment of a lunar control network is one of the core tasks in selenodesy, in which defining an absolute control point on the Moon is the most important step. However, up to now, the number of absolute control points has been very sparse. These absolute control points have mainly been lunar laser ranging retroreflectors, whose geographical location can be observed by observations on Earth and also identified in high resolution lunar satellite images. The Chang'e-3(CE-3) probe successfully landed on the Moon, and its geographical location has been monitored by an observing station on Earth. Since its positional accuracy is expected to reach the meter level, the CE-3 landing site can become a new high precision absolute control point. We use a sequence of images taken from the landing camera, as well as satellite images taken by CE-1 and CE-2, to identify the location of the CE-3 lander. With its geographical location known, the CE-3 landing site can be established as a new absolute control point, which will effectively expand the current area of the lunar absolute control network by 22%, and can greatly facilitate future research in the field of lunar surveying and mapping, as well as selenodesy.     

高精度国际时间比对的进展

在过去的４５ｙｒ中原子频标的性能大约每７ｙｒ提高一个数量级,从国际标准时间和各国高精度守时的需要出发,远距离的高精度时间频率传递比对技术也有与之相适应的很大的发展。ＧＰＳ卫星在近２０ｙｒ中不仅成为导航定位不可缺少的工具,在时间、频率的方面也发挥出巨大威力;近年来多通道“全视接收”技术的发展钎时频传输比对的稳定性有了重大改善;ＧＬＯＮＡＳＳ卫星系统在高精度时间比对方面正在成为ＧＰＳ系统的重要补充手段     

反常折射引起的地面天文观测残差的周年变化

我国光学天文观测有相当长历史，观测精度也较高，但是与国际系统相比。无论是测时还是测纬，所有仪器残差都有类似的周年变化，本文作者认为部分原因是由于我国季节变化引起的大气等密度层倾斜，从而产生的反常折射所引起的，文中对反常折射的规律进行了研究，导出了由于气象参数变化而引起的反常折射公式，并与测时，测纬的残差周年项进行了对比，结果表明用反常折射可以部分地解释我国天文观测残差的周年变化。     

Symplectic adaptive algorithm for solving nonlinear two-point boundary value problems in Astrodynamics

In this paper, from a Hamiltonian point of view, the nonlinear optimal control problems are transformed into nonlinear two-point boundary value problems, and a symplectic adaptive algorithm based on the dual variational principle is proposed for solving the nonlinear two-point boundary value problem. The state and the costate variables within a time interval are approximated by using the Lagrange polynomial and the costate variables at two ends of the time interval are taken as independent variables. Then, based on the dual variational principle, the nonlinear two-point boundary value problems are replaced by a system of nonlinear equations which can preserve the symplectic structure of the nonlinear optimal control problem. Furthermore, the computational efficiency of the proposed symplectic algorithm is improved by using the adaptive multi-level iteration idea. The performance of the proposed algorithm is tested by the problems of Astrodynamics, such as the optimal orbital rendezvous problem and the optimal orbit transfer between halo orbits.