武汉市人口集聚特征及其空间分异机制分析

当前人口集聚影响因素的研究多基于单因子影响力探讨,多因子及其交互作用方面的研究相对较少.鉴于此,本文以武汉市为例,引入地理探测器,分析不同因素和其交互作用对人口集聚的影响作用,为城市规划提供决策参考.结果表明:1)相比工作时段,休息时段人口相对分散,但中心空心化趋势不明显;2)从各因素的影响作用来看,第三产业企业密度、路网密度、房价、地铁站可达性等对人口集聚影响最大;3)人口集聚受到因子间交互作用影响明显,其中第三产业企业密度与房价以及第三产业企业密度与POI多样性的交互作用力最强.     

基于PS-InSAR技术的深圳北站表面位移监测研究

利用2015-01-2018-08的40景COSMO-SKyMed HIMAGE雷达影像,采用永久散射体合成孔径雷达干涉测量(permanent scatterers interferometric synthetic aperture radar,PS-InSAR)技术获得了深圳北站时序形变信息,并基于GIS空间分析方法进一步揭示了深圳北站表面位移的空间分布特征.根据InSAR遥感解译结果,结合深圳北站的工程建设背景,分析深圳北站表面位移的分布演化态势及其形变主导因素.结果表明,深圳北站东广场填土、填砂厚度以及土壤成分、力学性质发生了一定变化,造成缤果空间地基下沉,墙体出现裂缝,外在的高强度工程施工(汇德大厦)则进一步加剧了地面沉降.通过实地踏勘验证了InSAR监测结果的准确性,证实了高分辨率PS-InSAR技术在城市公共设施形变监测、管理维护方面的可行性.     

极移时间序列建模及预测

基于自回归滑动平均(auto-regressive and moving average,ARMA)模型以及一阶差分ARMA模型分别对极移的X分量和Y分量进行了模型拟合,并利用所拟合的模型对极移进行了预测.通过与国际地球自转服务发布的实测极移数据以及其他方法对比,证明了所建立的拟合模型在短期预报上的有效性.且X分量的ARMA模型在39 d预报跨度内的整体精度优于一阶差分ARMA模型,而Y分量45 d内的一阶差分ARMA模型预报精度比ARMA模型预报精度更高.     

基于惯性系原理的动基座粗对准及其性能影响因素分析

捷联惯导系统(strapdown inertial navigation system,SINS)在进行导航解算前需要粗对准提供初始姿态角,载体受多种因素影响和制约,在微幅晃动或运动状态下,需要进行动基座粗对准.从惯性系对准原理出发,讨论了基于比力和速度矢量的两种动基座粗对准解算方案,分析了位置误差、速度误差、杆臂误差对动基座粗对准的影响.结果表明,惯性系对准方法能够满足SINS粗对准的要求,速度误差和杆臂误差是制约对准精度与速度的主要因素,机动性强的轨迹能够加快对准速度,基于速度矢量的解算方案能够有效减弱姿态角收敛过程中的抖动,以提高对准效率.     

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.     

Secular tidal changes in lunar orbit and Earth rotation

Small tidal forces in the Earth–Moon system cause detectable changes in the orbit. Tidal energy dissipation causes secular rates in the lunar mean motion n, semimajor axis a, and eccentricity e. Terrestrial dissipation causes most of the tidal change in n and a, but lunar dissipation decreases eccentricity rate. Terrestrial tidal dissipation also slows the rotation of the Earth and increases obliquity. A tidal acceleration model is used for integration of the lunar orbit. Analysis of lunar laser ranging (LLR) data provides two or three terrestrial and two lunar dissipation parameters. Additional parameters come from geophysical knowledge of terrestrial tides. When those parameters are converted to secular rates for orbit elements, one obtains dn/dt = \(-25.97\pm 0.05 ''/\)cent\(^{2}\), da/dt = 38.30 ± 0.08 mm/year, and di/dt = ?0.5 ± 0.1 \(\upmu \)as/year. Solving for two terrestrial time delays and an extra de/dt from unspecified causes gives \(\sim \) \(3\times 10^{-12}\)/year for the latter; solving for three LLR tidal time delays without the extra de/dt gives a larger phase lag of the N2 tide so that total de/dt = \((1.50 \pm 0.10)\times 10^{-11}\)/year. For total dn/dt, there is \(\le \)1 % difference between geophysical models of average tidal dissipation in oceans and solid Earth and LLR results, and most of that difference comes from diurnal tides. The geophysical model predicts that tidal deceleration of Earth rotation is \(-1316 ''\)/cent\(^{2}\) or 87.5 s/cent\(^{2}\) for UT1-AT, a 2.395 ms/cent increase in the length of day, and an obliquity rate of 9 \(\upmu \)as/year. For evolution during past times of slow recession, the eccentricity rate can be negative.     

Line-of-Sight Anisotropies in the Cosmic Dawn and Epoch of Reionization 21-cm Power Spectrum

The line-of-sight direction in the redshifted 21-cm signal coming from the cosmic dawn and the epoch of reionization is quite unique in many ways compared to any other cosmological signal. Different unique effects, such as the evolution history of the signal, non-linear peculiar velocities of the matter etc. will imprint their signature along the line-of-sight axis of the observed signal. One of the major goals of the future SKA-LOW radio interferometer is to observe the cosmic dawn and the epoch of reionization through this 21-cm signal. It is thus important to understand how these various effects affect the signal for its actual detection and proper interpretation. For more than one and half decades, various groups in India have been actively trying to understand and quantify the different line-of-sight effects that are present in this signal through analytical models and simulations. In many ways the importance of this sub-field under 21-cm cosmology have been identified, highlighted and pushed forward by the Indian community. In this article, we briefly describe their contribution and implication of these effects in the context of the future surveys of the cosmic dawn and the epoch of reionization that will be conducted by the SKA-LOW.