北京市房地产价格空间分布变化研究

针对北京市主城区房地产价格长区间的空间分布变化及其成因进行研究,为北京市房价的空间分布规律提供参考.采用空间相关性分析方法中的平均最近邻分析、全局Moran'sI指数、Moran散点图和LISA集聚图等分析工具结合空间自相关理论对北京市主城区房地产价格的空间分布变化进行分析,通过克里金插值分析方法验证房价的空间特征,分析空间分布的变化及其成因.得出北京市主城区房地产价格20152019年,空间集聚特征不变,正向空间自相关增强,价格中心由单中心变为中心—副中心的多中心形式,区位因素和交通可达性条件是影响房价空间分布变化的重要因素.     

改进特征金字塔网络的遥感影像崩滑体提取

针对大多数网络存在精度低,特征冗余,计算量大,训练时间长等问题,提出密集连接特征金字塔网络(DCFPN),将特征提取网络得到的特征图通过一组并行深度可分离空洞卷积进一步计算其全局语义信息,并搭建解码上采样网络,加入连接组合特征层的结构,对遥感影像进行语义分割实现崩滑体提取,较好地解决了参数量过多,计算时间较长和精度较低等问题.通过特征金字塔网络(FPN)和DCFPN在崩滑体数据集上的大量对比实验表明,DCFPN在崩滑体语义分割方面有更高的精度并且计算量更少,训练时间更短,能够更好地为应急抢险工作.     

玛河流域景观生态风险评价与时空分异

以玛纳斯河流域作为研究区,结合特殊的干旱区山地-绿洲-荒漠系统(Mountain-Oasis-Desert System简称MODS),综合考虑遥感影像数据光谱信息和纹理特征,将研究区分为耕地、林地、草地、水体、裸地、居民地、工业用地和冰川/永久积雪等8个景观类型,利用FRAGSTATS软件计算景观指数,引入生态风险的指数,将研究区划为低、较低、中、较高、高生态风险区五级,评估其景观格局的生态风险时空变化特征。结果表明:1)1990—2015年间,玛纳斯河流域景观变化主要表现为耕地、建设用地的增加以及水体、冰川/永久积雪面积的缩减;2)玛纳斯河流域的景观生态风险等级空间分布具有明显的差异,较低风险区的面积变化较为明显,低、较低生态的风险区比重有所上升,除此以外,林、草地类型各生态风险的等级所占比重的起伏波动具有明显的差异。建议应当合理地利用土地资源,尽量保护林地、草地等景观脆弱行较低的原生景观类型,禁止为开垦耕地而破坏林地、草地;增加土地的利用效率,更要对高等、较高生态风险区加强监管。     

结合地理空间数据的输电线路通道潜在滑坡体稳定性评价

输电线路常需要通过地质灾害危险区域,对输电线路通道所经区域的潜在滑坡体进行稳定性分析及安全评价具有重要意义.本文基于直升机扫描LiDAR DEM和DOM数据,利用地理空间信息处理技术和有限元强度折减法分析,对某输电线路通道潜在滑坡安全隐患的边坡进行了分析计算.首先对输电线路通道原始扫描数据进行处理,提取滑坡体参数,再通过有限元软件建立滑坡体的三维地质模型;然后,利用强度折减法对潜在滑坡体进行自然、暴雨工况下的数值模拟和稳定性计算,求出滑坡体的安全系数,获得滑坡体应力、应变和位移云图,综合评价线路通道潜在滑坡体的稳定状态,为输电线路电力设施通道滑坡灾害防治安全设计和施工提供科学依据.     

油气管道纵断数据自动提取技术研究

作为管道工程勘测设计中的一项重要工作,纵断面测量内业数据处理具有工作量大、自动化水平低的特点,极大地影响了工作效率.针对此问题,本文设计了油气管道纵断数据提取程序,实现油气管道中线高程点加密、基于机载LiDAR点云数据的纵断数据提取、里程和角度计算等功能,并应用在实际工作当中.该系统具有易操作、高精度、高效率等优势,大幅度提高了油气管道纵断面测量的工作效率.     

改进的AKAZE特征提取的全局式SFM三维重建算法

针对增量式SFM算法过渡依赖初始图像的选择,重建时误差累积导致场景漂移且计算效率低的问题,设计了一种改进的加速KAZE特征提取的全局式SFM三维重建算法.首先通过增强特征接受阈值并构造非线性尺度空间来提取图像的特征,使用改进局部差分二进制MLDB描述符对特征进行描述;然后利用全局式SFM算法对整个场景的相机位姿进行估计,从而减小误差并减少光束法平差BA的使用次数,降低了算法的复杂度,大大提高计算效率;最后利用基于面元的多视立体匹配PMVS算法得到稠密重建结果.实验结果表明,同等条件下该方法能够得到更多的有效点对,计算效率约为增量式SFM算法的2倍,且特征匹配准确率提高5％,稠密重建的点云精度高,信息丰富且纹理清晰,是一种有效的三维重建方法.     

Complex organics in space from Solar System to distant galaxies

Recent observational and experimental evidence for the presence of complex organics in space is reviewed. Remote astronomical observations have detected \(\sim \)200 gas-phased molecules through their rotational and vibrational transitions. Many classes of organic molecules are represented in this list, including some precursors to biological molecules. A number of unidentified spectral phenomena observed in the interstellar medium are likely to have originated from complex organics. The observations of these features in distant galaxies suggests that organic synthesis had already taken place during the early epochs of the Universe. In the Solar System, almost all biologically relevant molecules can be found in the soluble component of carbonaceous meteorites. Complex organics of mixed aromatic and aliphatic structures are present in the insoluble component of meteorites. Hydrocarbons cover much of the surface of the planetary satellite Titan and complex organics are found in comets and interplanetary dust particles. The possibility that the early Solar System, or even the early Earth, have been enriched by interstellar organics is discussed.     

The realm of the galaxy protoclusters

The study of galaxy protoclusters is beginning to fill in unknown details of the important phase of the assembly of clusters and cluster galaxies. This review describes the current status of this field and highlights promising recent findings related to galaxy formation in the densest regions of the early universe. We discuss the main search techniques and the characteristic properties of protoclusters in observations and simulations, and show that protoclusters will have present-day masses similar to galaxy clusters when fully collapsed. We discuss the physical properties of galaxies in protoclusters, including (proto-)brightest cluster galaxies, and the forming red sequence. We highlight the fact that the most massive halos at high redshift are found in protoclusters, making these objects uniquely suited for testing important recent models of galaxy formation. We show that galaxies in protoclusters should be among the first galaxies at high redshift making the transition from a gas cooling regime dominated by cold streams to a regime dominated by hot intracluster gas, which could be tested observationally. We also discuss the possible connections between protoclusters and radio galaxies, quasars, and \(\hbox {Ly}\alpha \) blobs. Because of their early formation, large spatial sizes and high total star-formation rates, protoclusters have also likely played a crucial role during the epoch of reionization, which can be tested with future experiments that will map the neutral and ionized cosmic web. Lastly, we review a number of promising observational projects that are expected to make significant impact in this growing, exciting field.     

Dynamics of the Jupiter Trojans with Saturn’s perturbation when the two planets are in migration

In a previous paper (Hou et al. in Celest Mech Dyn Astron 119:119–142, 2014a), the problem of dynamical symmetry between two Jupiter triangular libration points (TLPs) with Saturn’s perturbation in the present configuration of the two planets was studied. A small short-time scale spatial asymmetry exists but gradually disappears with the time going, so the planar stable regions around the two Jupiter TLPs should be dynamically symmetric from a longtime perspective. In this paper, the symmetry problem is studied when the two planets are in migration. Several mechanisms that can cause asymmetries are discussed. Studies show that three important ones are the large short-time scale spatial asymmetry when Jupiter and Saturn are in resonance, the changing orbits of Jupiter and Saturn in the planet migration process, and the chaotic nature of Trojan orbits during the planet migration process. Their joint effects can cause an observable difference to the two Jupiter Trojan swarms. The thermal Yarkovsky effect is also found to be able to cause dynamical differences to the two TLPs, but generally they are too small to be practically observed.     

Integrability of motion around galactic razor-thin disks

We consider the three-dimensional bounded motion of a test particle around razor-thin disk configurations, by focusing on the adiabatic invariance of the vertical action associated with disk-crossing orbits. We find that it leads to an approximate third integral of motion predicting envelopes of the form \(Z(R)\propto [\varSigma (R)]^{-1/3}\), where R is the radial galactocentric coordinate, Z is the z-amplitude (vertical amplitude) of the orbit and \(\varSigma \) represents the surface mass density of the thin disk. This third integral, which was previously formulated for the case of flattened 3D configurations, is tested for a variety of trajectories in different thin-disk models.