基于星通软件的农村土地承包经营权确权登记颁证数据处理

更新地籍信息对于记录土地所有权和财产分割的变化至关重要,在大多数情况下,现有的宗地图不能提供关于地块边界的最新信息,因此,需要及时提供地籍图中的地籍数据和地块边界信息。本文以安徽省一个行政村土地承包经营权确权登记颁证为研究对象,以星通承包经营权采编系统(以下简称星通软件)在土地确权颁证登记中的应用为研究内容,通过实践表明,星通软件为农村土地确权内业数据处理带来了极大的便利。     

三维虚拟仿真的学生校园活动监控系统

针对目前校园安保监控措施脆弱的实际问题,以及积极推动我国智慧城市建设的实际需求,以中南大学新校区为实验区,基于CityEngine软件的快速建模方法与WebGIS三维模型渲染技术,使用Java语言开发了基于三维虚拟仿真的学生校园活动监控系统。该系统不仅可以进行校园的三维场景动画漫游,还提供了基于学生实时手机定位的监控功能。     

一种基于复合金字塔模型的三维模型数据组织方法

针对异构三维模型数据的统一组织和集成管理问题,本文以目前主流金字塔模型、三维场景瓦片的数据组织方法和地图服务规范等相关技术为基础,提出了一种基于复合金字塔模型的三维模型数据组织方法。该方法首先构建覆盖测区的地理格网模型,以此作为异构三维模型数据集成的空间框架。其次,建立三维模型数据与地理格网单元的映射关系,从而构建复合金字塔模型,实现异构三维模型数据的统一管理。最后,在数据结构上对现有数据格式进行扩展,设计了一种面向网络传输的数据格式储存三维模型数据,完成异构三维模型数据的一体化存储。试验结果表明,该方法能够实现异构三维模型数据统一组织与集成管理。     

球面距离计算方法及精度比较

球面距离(角间距)计算是天文或地理学中极常用的计算之一,也是目标查找、锥形检索、交叉证认等方法的基础。数学上,通过球面几何可以直接计算出两点的距离,前人已经推导出了多个复杂程度不一的计算方法。但是由于计算机的精度有限,在进行数值计算时有舍入误差,导致公式计算结果出现偏差。对几个常用的球面距离计算公式进行了考察,测试并对比它们在不同计算环境下的精度与优缺点。此外还展示并比较了几种常用天文软件包、数据库的球面距离计算方法,以期有助于天文工作者选择适合自己当前需要的计算方法。     

耀变体在射电波段的偏振研究

利用UMRAO数据库22个耀变体源的偏振数据,根据Lazarian&Pogosyan理论模型分析研究了耀变体射电波段的偏振随波长的变化,得出不同类的耀变体偏振随波长变化的原因。结果表明,与Lazarian&Pogosyan理论模型吻合较好。由此得出如下结论:(1)反常去偏振耀变体源中反常法拉第旋光起主导作用,反常去偏振相对较少;(2)热辐射与同步辐射混合作用,高频波段的偏振度小于低频波段的偏振度(反常去偏振);(3)当被观测波段波长小于吸积盘热辐射对应的维恩波长时,高频波段的偏振度大于低频波段的偏振度(常规去偏振)。     

南山26米射电望远镜轨道高差测量及其对指向精度的影响

轮轨式天线的轨道作为承载整个天线重量的基础,其精度直接影响天线在方位方向运转的平稳性,引起天线轴系偏差从而影响天线的指向精度。介绍改造后的乌鲁木齐南山26 m射电望远镜(Nanshan Radio Telescope, NSRT)轨道结构以及轨道高差测量,并建立天线在不同方位、俯仰角下轨道高差引起天线指向偏差的数学模型。利用"十字扫描"法实测多颗标准源在相应位置的指向数据,并通过高斯拟合得到指向偏差。通过分析可知,轨道高差引起的指向偏差经过修正可以提高天线的指向精度。     

天文CMOS相机测试平台及控制系统的实现

CMOS相机是一种重要的固体成像设备?随着科研级CMOS相机的性能不断提高,现已广泛应用于科研领域?新真空太阳望远镜的成像设备也使用CMOS相机?因此建立一个天文CMOS相机测试系统?对于新购CMOS相机的验收以及现有CMOS相机的定期检测和维护有十分重要的意义。介绍了CMOS相机测试平台的硬件组成,并针对实际测试中对设备控制的需求,以及利用控制器对相应的设备直接控制,提出了基于TCP/IP协议以及串口通信的设计方案?利用C#编程语言设计了一套多线程并行的控制系统软件?实现各设备在局域网内的远程并行控制。通过对设备的运行测试,结果表明,系统能良好地控制各设备的正常运行?满足测试系统集成控制的需求.     

The symmetry energy and incompressibility constrained by the observations of glitching pulsars

We investigate the masses of glitching pulsars in order to constrain their equation of state(EOS). The observations of glitches(sudden jumps in rotational frequency) may provide information on the interior physics of neutron stars. With the assumption that glitches are triggered by superfluid neutrons, the masses of glitching neutron stars can be estimated using observations of maximum glitches.Together with the observations of thermal emission from glitching pulsars Vela and J1709–4429, the slope of symmetry energy and incompressibility of nuclear matter at saturation density can be constrained.The slope of symmetry energy L should be larger than 67 MeV while the lower limit of incompressibility for symmetric nuclear matter K_0 is 215 MeV. We also obtain a relationship between L and K_0:6.173 MeV + 0.283 K_0≤ L ≤ 7.729 MeV + 0.291 K_0. The restricted EOSs are consistent with the observations of 2-solar-mass neutron stars and gravitational waves from a binary neutron star inspiral.     

Orbital evolution of a planet with tidal dissipation in a restricted three-body system

The angle between planetary spin and the normal direction of an orbital plane is supposed to reveal a range of information about the associated planetary formation and evolution. Since the orbit's eccentricity and inclination oscillate periodically in a hierarchical triple body and tidal friction makes the spin parallel to the normal orientation of the orbital plane with a short timescale in an isolated binary system, we focus on the comprehensive effect of third body perturbation and tidal mechanism on the angle. Firstly, we extend the Hut tidal model(1981) to the general spatial case, adopting the equilibrium tide and weak friction hypothesis with constant delay time, which is suitable for arbitrary eccentricity and any angle ? between the planetary spin and normal orientation of the orbital plane. Furthermore, under the constraint of angular momentum conservation, the equations of orbital and ratational motion are given. Secondly, considering the coupled effects of tidal dissipation and third body perturbation, and adopting the quadrupole approximation as the third body perturbation effect, a comprehensive model is established by this work. Finally, we find that the ultimate evolution depends on the timescales of the third body and tidal friction. When the timescale of the third body is much shorter than that of tidal friction, the angle ? will oscillate for a long time,even over the whole evolution; when the timescale of the third body is observably larger than that of the tidal friction, the system may enter stable states, with the angle ? decaying to zero ultimately, and some cases may have a stable inclination beyond the critical value of Lidov-Kozai resonance. In addition, these dynamical evolutions depend on the initial values of the orbital elements and may aid in understanding the characteristics of the orbits of exoplanets.     

The galaxy luminosity function in the LAMOST Complete Spectroscopic Survey of Pointing Area at the Southern Galactic Cap

We present optical luminosity functions(LFs) of galaxies in the~(0.1) g,~(0.1) r,~(0.1) i bands, calculated using data in~40 deg~2 sky area of the LAMOST Complete Spectroscopic Survey of Pointing Area(LaCoSSPAr) in the Southern Galactic Cap. Redshifts for galaxies brighter than r = 18.1 were obtained mainly with LAMOST. In each band, LFs derived using both parametric and non-parametric maximum likelihood methods agree well with each other. In the0.1 r band, our fitting parameters of the Schechter function are φ_*=(1.65 ± 0.36) × 10~(-2) h~3 Mpc~(-3), M_*=-20.69 ± 0.06 mag and α =-1.12 ± 0.08,which agree with previous studies. Separate LFs are also derived for emission line galaxies and absorption line galaxies. The LFs of absorption line galaxies show a dip at~(0.1) r ~18.5 and can be fitted well by a double-Gaussian function, suggesting a bimodality in passive galaxies.