高精度高性价比的GPS定向仪的设计

介绍了一种高精度、高性价比的GPS定位定向仪的设计及实现（〈1mil,2σ）方法,系统利用了实际应用中的有利约束条件,对基于LAMBDA方法的载波相位整周模糊度解算算法进行了改进,经过系统工程设计,在实际应用中实现了单频、高精度、快速定向数据的输出。可以满足绝大多数环境下的使用需求,大大降低了系统成本。     

蛋白质营养对高密度养殖凡纳滨对虾生长与免疫力的影响

在高密度养殖条件下,进行单因素随机设计动物试验.用5种饲料(蛋白质水平31%、35%、39%、43%、47%,以A～E组表示)分别投喂平均体质量6.2 g+0.2 g、平均养殖密度3.1 kg/m3的凡纳滨对虾(Litopenaeus vannamei),探寻蛋白质营养对虾生长、免疫、水质、抗胁迫的影响特征.结果表明:(1)中高蛋白质水平具有显著促进对虾生长的效果,随着蛋白水平的提高,特定生长率先增加后降低,饲料系数正好相反,D组两指标最佳,分另q为110.98%和2.54;C、D、E组差异不显著.(2)中高蛋白质水平有利于提高对虾多数免疫指标的活力,血淋巴中血细胞浓度、T-AOC活力、POD活力、总蛋白含量、白蛋白、血蓝蛋白含量,随着蛋白质水平提高先增加后降低,前5指标含量均以D组最高,比A组显著提高16.8%～33.9%;而血蓝蛋白含量C组最高,比A组提高15.0%.(3)高蛋白质水平有利于提高对虾SOD活力,也显著增强抗低盐胁迫的能力,但同时极显著加大了水环境中氨氮和亚硝氮的污染.(4)在我国北方集约化高密度养殖条件下,凡纳滨对虾中后期生长阶段适宜的饲料蛋白质营养水平为39%～43%.     

桩板组合结构的技术特点及应用

介绍了桩板组合结构的组成和特点,及其在实际工程中的应用。该结构可作为滩海地区进海路路堤、人工岛护壁、保滩促淤丁坝和离岸堤主体结构。     

复合型滑坡体系统的工程地质勘察及其稳定性分析

滑坡工程地质勘察及其稳定性分析是滑坡治理工程设计及施工的重要依据.国道316线福建境内K160+840~K161+020山体滑坡是由2个主滑动轴线所构成的复合滑坡体,它具有牵引和推移性质特征,发育2个主滑动面和2个次滑动面.详细论述了复合滑坡体工程地质勘察的内容及侧重点.该滑坡体自然状态下的稳定系数为1.025,处于临界稳定状态,但安全储备极低,必须及早进行工程治理.     

Comparison of chaos detection methods in the circular restricted three‐body problem

In this study, a sample of orbits is considered in the framework of the planar circular restricted three‐body problem. In order to separate ordered from chaotic orbits three numerical methods are compared: the Largest Lyapunov Characteristic Exponent (LLCE) and the Smaller Alignment Index (SALI) provide a fairly good characterization of the chaotic motions, while the computational time required is of the same order; the Correlation Dimension (CD) has the advantage of correctly classifying sticky orbits, but at the expense of a longer computational time. In order to classify a given orbit, any pair of the three methods can be considered, but LLCE and SALI are recommended due to their speed. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Symbiotic stars with spectral indication of bipolar ejection and stellar wind

Four out of a total of five symbiotic systems whose optical spectral lines contain satellite components indicating collimated ejection have an additional absorption of P Cyg type with different velocity. These systems are Z And, Hen 3‐1341, StHα 190, and BF Cyg. It is shown that the line profiles of every of these systems can be interpreted in the framework of a model of a collimated stellar wind from the hot compact component proposed initially to interpret the line profiles of Z And, observed during its last active phase after 2000. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

3XMM J185246.6+003317 as transient neutron star

We performed an X‐ray timing and spectral analysis of the variable source 3XMM J185246.6+003317 to investigate its physical nature. The data from all observations of 3XMMJ185246.6+003317 conducted by XMM‐Newton EPIC MOS1 and MOS2 with the same instrumental setup in 2004–2009 were reprocessed to form a homogenous data set of solar barycenter corrected photon arrival times and high S/N spectra of 3XMM J185246.6+003317. A Bayesian method for the search, detection, and estimation of the parameters of a periodic signal of unknown shape was employed, as developed by Gregory & Loredo (1992, 1993). The results show that 3XMM J185246.6+003317 is a transient neutron star with the genuine spin‐period of 23.11722 (23.11711–23.11727) s and its derivative of 5.3(0.3–5.5)×10^–11 s s^–1, implying a characteristic age of 7 (6–104) kyr, if the period derivative can be ascribed to the genuine spin‐down rate of the neutron star. The rotational‐phase averaged X‐ray spectra at the different brightness periods can be fitted with a highly absorbed blackbody model with different temperatures. The phase‐folded light curves in different energy bands with high S/N ratio show a double‐peaked profile; the variations depend on time and energy, indicating that radiation emerges from at least two emitting areas. The spectra at the phases corresponding to the maxima in the phase‐folded light curve show different spectral parameters of absorbed blackbody radiation, i.e. the hotter one has a smaller size. The source is detected only from September 2008 to April 2009 with persistently decreasing brightness, but not before, even though it was observed by XMM. Hence, it is a transient neutron star or a binary system hosting it. (© 2015 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Clusters and groups of galaxies in the 2dF galaxy redshift survey: A new catalogue

We create a new catalogue of groups and clusters, applying the friends‐of‐friends method to the 2dF GRS final release. We investigate various selection effects due to the use of a magnitude limited sample. For this purpose we follow the changes in group sizes and mean galaxy number densities within groups when shifting nearby observed groups to larger distances. We study the distribution of sizes of dark matter haloes in N ‐body simulations and compare properties of these haloes and the 2dF groups. We show that at large distances from the observer luminous and intrinsically greater groups dominate, but in these groups only very bright members are seen, which form compact cores of the groups. These two effects almost cancel each other, so that the mean sizes and densities of groups do not change considerably with distance. Our final sample contains 10750 groups in the Northern part, and 14465 groups in the Southern part of the 2dF survey with membership N _gal ≥ 2. We estimate the total luminosities of our groups, correcting for group members fainter than the observational limit of the survey. The cluster catalogue is available at our web‐site ( http://www.aai.ee/∼maret/2dfgr.html ). (© 2006 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)