地面GPS观测探测大气可降水汽量的方法和前景

介绍了利用地面GPS观测探测大气可降水汽量（PWV）的基本原理和方法及其在气象学和天文定位上的应用．地面GPS测量的PWV估计的主要误差源来自天顶湿延迟的估计．为了提高天顶湿延迟的估计精度,根据大气湿分量随时间变化的特性,天顶湿延迟的估算可采用确定性参数估计和随机模型估计．采用这些方法能有效地提高GPS精密定位中高程测量的精度,且其估算的PWV的精度可达1-2mm,足以满足天气预报和气候研究的需要．简述了大气分布的非球对称性对PWV估计的影响并评述了利用地面GPS测量探测PWV的前景．     

电离层延迟改正对GPS定时的影响分析

为分析电离层延迟改正对GPS定时的影响,采用修正电离层延迟的Klobuchar模型法和双频法,并利用IGS(International GNSS Service)观测站多天的GPS实测数据,计算得到了定位结果、GPS接收机钟差及其与IGS产品的测站钟差之差值.计算结果的分析表明,上述两种电离层延迟修正法有利于改善GPS定时结果,其中双频改正法效果更好.     

提高中性大气折射延迟改正精度的可能途径

针对空间大地测量技术对中性大气折射延迟改正精度的要求,阐述了折射延迟改正值应随测站和随方位而异的必要性．指出,在尚不能直接测定天文大气折射值的情况下,现有的各种改正模型对大气分布模型的依赖性,不能达到预期的精度和降低观测的截止角．根据云南天文台低纬子午环的特殊结构,和测定大气折射的实践,提出了提高折射延迟改正精度的新方法,即：利用各观测站不同方位从天顶附近直到低地平高度角的天文大气折射实测数据,求解得到折射率差和映射函数的参数,从而建立随测站和随方位而异的大气折射延迟改正模型．这一新方法的实施,将能在不需采用大气分布模型的情况下,把天顶延迟的改正精度提高到1 mm以内,低地平高度角的折射延迟改正精度提高到厘米级,并且把截止高度角压缩到5°以内．     

GNSS对流层延迟映射模型分析

介绍了GNSS定位中常用的三种对流层映射函数NMF、GMF、VMF1和一种新的模型——GPT2,通过测站气压、天顶静力学延迟分量以及投影函数参数三个方面对这几个模型进行了比较。采用不同的模型对全球均匀分布的30个IGS测站2012年全年的GPS观测数据进行精密单点定位,分析了不同模型解算的测站坐标与对流层天顶延迟精度。分析结果表明:以实测气压为基准,VMF1模型气压误差仅为0.4%,GPT2模型相对于GPT模型改善了约25%;以VMF1 HT模型为基准,GPT和GPT2模型天顶静力学延迟中误差约为1 cm,GPT2模型精度略优于GPT模型;以VMF1网站发布的测站VMF1模型为基准,GPT2模型的干、湿映射函数参数ah、aw中误差约为1×10-5和5×10-5;在IGS08框架下,GMF/GPT与VMF1/GPT2模型的PPP坐标解精度比NMF提高了22%;两模型定位精度与ZTD精度都明显高于NMF模型。     

上海天文台GPS气象学的研究现状

介绍了上海天台GPS气象学的背景,进展和研究成果,从90年代起,上海天台就分别开展了地基GPS气象学和空基GPS气象学的研究工作,在地基GPS气象研究中,利用国内分布的23个GPS网站及周边地区6个IGS台站,在1996年7月26日到31日（6天）的GPS观测资料,首先求得中性大气天顶延迟改正序列,然后推出测站上空可降水汽量积分,采样频率分别取为30分钟和2小时,得到的天顶延迟改正的精度好于1cm,后演出可降不汽含量的内部精度约1－2mm,把国内GPS网中具有探空气球观测的4个台站,上海,武汉,箍春和西宁的资料进行比较,发现GPS和探空气球的可降水汽含量之间的平均中误差为3－4mm,考虑到上海地区在台风和气候变化较剧烈的季节因素,选择了1997年8月2日到9日（8天）和8月17日至27日（11天）的两个观测时段,做了国内第一个GPS/storm实验,实验结果表明,地面GPS网有可能获得几乎实时的,连续的和主精度的可降水汽含量值,它的结果很好地与实时降雨量过程相对应,实验证明,利用预报轨道可以获得与精密轨道几乎相同的结果,在空基GPS气象研究中,发现地面GPS网水汽观测具有良好的时间覆盖率的优点,缺乏空间分辨率的缺点,而现在的GPS无线电掩星方法恰恰具有良好的空间分辨率而缺乏时间覆盖率,因此,在地球低轨道（LEO）卫星的轨道设计中,提出了通约LEO卫星的方法,希望通过改进轨道的LEO卫星获得长达200多天的观测序列,而它的地面观测点的漂移可以控制在于小100km,这种方法也可以用来设计对特定地面点上空大气剖面的测定,还在设计和建立GPS无线电掩星反演大气剖面的软件。     

基于高精度对流层延迟改正的转发式卫星测定轨

转发式卫星测定轨传统上一直使用气象站数据和Saastamonien模型,计算天顶对流层延迟,精度约为4 cm。为了提高对流层延迟改正精度,并进一步提高卫星测定轨精度,在转发式测轨站上并址配置测地型GPS/BDS多系统接收机,基于IGS/iGMAS产品计算得到各站高精度的对流层天顶延迟,精度约为5 mm。将此新的对流层延迟改正应用于定轨软件,开展了GEO卫星转发式测定轨试验。试验结果表明:使用本文方法的对流层延迟后,定轨精度有较为明显提高,平均重叠弧段轨道差由1.402 m,减小到1.268 m,改善约为10%。     

三种对流层延迟改正模型精度评估

利用36个全球分布的IGS站2003全年GPS实测的对流层天顶延迟数据和气象数据,对目前国内外常用的两个对流层延迟改正模型;Hopfield模型、Saastamoinen模型和最近几年发展起来的EGNOS模型的改正精度和适用范围进行评估,指出Hopfield模型在应用中存在的缺陷,EGNOS模型可用作GNSS实时定位和导航的对流层天顶延迟的改正模型.     

GPS精密定位中对流层折射参数估计方法的比较分析

利用GPS实测资料，对GPS相对定位中对流层折射天顶延迟参数估计方法的单参数法、分段常数法和分段线性法进行了分析，讨论了各种方法的参数估计结果和对相对定位结果的影响。指出单参数方法存在较大的误差，这一误差主要影响基线垂直分量的精度，用分段常数法和分段线性法可明显提高基线垂直分量上的重复率，但这一精度的提高并非随分段数的增加而单调增加，各测站应分别选用各自最合适的模拟估计方法和分段数，才是最合理的。     

1.56米望远镜的极轴校正和跟踪误差测定方法与结果

1.56米天望远镜已于1989年上海天台的佘山工作站投入使用，经校正，瓣极轴指向偏离北极为：0″.±4″.48（在方位上）和0″.±2″.21（在高度上）。望远镜的跟踪误差也被测定：在天顶附近30分钟内所作的128次观测得到的望远镜跟踪的均方根误差为±0″.36。结果表明，1.56米望远镜的恒动跟踪十分优良。     

分析昆明GPS站相对欧亚板块的运动

利用国际联测和综合处理 ,得到昆明GPS站地壳形变速率每年以( -4 .3± 0 .5)mm下沉趋势 ,水平分别以 3 7.5mm ,方位 1 47°± 1 .°5运动。利用最新国际地球自转服务 (IERS)发布的国际地球参考架ITRF2 0 0 0速度场 ,建立最新反映全球板块模型 ,基于最新的ITRF2 0 0 0地球参考架和欧亚板块的欧拉矢量 ,估计得到昆明站的地壳垂直形变速率为每年 -0 .0 1mm呈下降趋势 ,水平形变速率为每年 ( 8.1± 0 .2 0 )mm ,方位 1 3 7°± 1 .°5;并进一步分别基于几百万年地质地磁模型NNR -NUVEL1A和ITRF96、ITRF97模型的欧亚板块的欧拉矢量 ,得到较一致的结果 ,说明全球板块运动稳定性与模型的可靠性。本文基于不同板块模型分析了昆明GPS站相对于欧亚板块运动     

A survey of orbits of co-orbitals of Mars

Many asteroids with a semimajor axis close to that of Mars have been discovered in the last several years. Potentially some of these could be in 1:1 resonance with Mars, much as are the classic Trojan asteroids with Jupiter, and its lesser-known horseshoe companions with Earth. In the 1990s, two Trojan companions of Mars, 5261 Eureka and 1998 VF₃₁, were discovered, librating about the L₅ Lagrange point, 60° behind Mars in its orbit. Although several other potential Mars Trojans have been identified, our orbital calculations show only one other known asteroid, 1999 UJ₇, to be a Trojan, associated with the L₄ Lagrange point, 60° ahead of Mars in its orbit. We further find that asteroid 36017 (1999 ND₄₃) is a horseshoe librator, alternating with periods of Trojan motion. This asteroid makes repeated close approaches to Earth and has a chaotic orbit whose behavior can be confidently predicted for less than 3000 years. We identify two objects, 2001 HW₁₅ and 2000 TG₂, within the resonant region capable of undergoing what we designate “circulation transition”, in which objects can pass between circulation outside the orbit of Mars and circulation inside it, or vice versa. The eccentricity of the orbit of Mars appears to play an important role in circulation transition and in horseshoe motion. Based on the orbits and on spectroscopic data, the Trojan asteroids of Mars may be primordial bodies, while some co-orbital bodies may be in a temporary state of motion.     

Equation of state and anisotropy of pressure of magnetars

Magnetars are the neutron stars with the highest magnetic fields up to 10¹⁵–10¹⁶ G. It has been proposed that they are also responsible for a variety of extra-galactic phenomena, ranging from giant flares in nearby galaxies to fast radio bursts. Utilizing a relativistic mean field model and a variable magnetic field configuration, we investigate the effects of strong magnetic fields on the equation of state and anisotropy of pressure of magnetars. It is found that the mass and radius of low-mass magnetars are weakly enhanced under the action of the strong magnetic field, and the anisotropy of pressure can be ignored. Unlike other previous investigations, the magnetic field is unable to violate the mass limit of the neutron stars.     

Estimation of the Time Scale of Merging of the Components of Contact Binaries of the W UMa Type

Time scales of the transition from contact binary systems of the W UMa type to single stars of the blue straggler type are estimated. A model of one-way mass transfer from the primary component to the companion inside a common envelope (Eggen et al.) and a model of a contact binary lying on the zero-age main sequence with a companion that is losing mass (F. van't Veer) are used to calculate these scales. The merging times of components were calculated for 304 contact systems of the W UMa type from the Catalog of Approximate Photometric and Absolute Elements of Eclipsing Variable Stars on a scale of loss of mass and orbital angular momentum due to magnetic braking, under the assumption of synchronization of the axial rotation and orbital revolution. On the basis of the resulting statistics, the characteristic merging scales are 0.4-0.6 and 0.5-0.7 Gyr, respectively, for the above two models. The results of a comparison with the work of other authors are discussed.     

Modeling of lightcurves of binary asteroids

We present a numerical method for inverting long-period components of lightcurves of asynchronous binary asteroids. Data of five near-Earth binary asteroids, (175706) 1996 FG₃, (65803) Didymos, (66391) 1999 KW₄, (185851) 2000 DP₁₀₇ and (66063) 1998 RO₁, for two of them from more than one apparition, were inverted. Their mutual orbits' poles and Keplerian elements, size ratios, and ellipsoidal shape axial ratios were estimated via this inversion. The pole solutions and size ratios for 1999 KW₄ and 2000 DP₁₀₇ are in a good agreement with independent estimates from radar measurements. We show that uncertainties of estimates of bulk densities of binary systems can be large, especially when observed on short arcs.     

Investigation of Times of Minima of Selected Early-Type Eclipsing Binaries

New precise times of minimum light for several early-type eclipsing binaries were obtained at three observatories. The changes of period of the following measured binaries are discussed: V1182 Aql, LY Aur, SZ Cam, FZ CMa, QZ Car, LZ Cen, V606 Cen, AH Cep and TU~Mus.     

Flattening of galaxies of different morphological types in subclusters of Coma

This paper deals with the observed variation in the flattening of galaxies with the density of galaxies in the subclusters of Coma surrounding NGC 4889, NGC 4874, and NGC 4839 based on data from the Abastumani Combined Catalog of Galaxies. The mean values of the observed ratios of the diameters of the galaxies, as well as histograms of their distributions, indicate that in the central, dense regions of the subclusters within a volume of 0.5h ₇₅ ⁻¹ Mpc³, E and S0 type galaxies are close to spheroidal. A significant reduction in the mean values of the diameters of the galaxies in the subclusters is noted, regardless of their morphology relative to the galaxies in the halo of the Coma cluster. In the subclusters, spiral galaxies are found with a hydrogen deficit that is more than 5 times the hydrogen deficit in spirals within the halo of the cluster. According to their 3-D coordinates, most of the galaxies with a hydrogen deficit are located closer to the south-east edge of the subcluster surrounding NGC 4874 near an extended gas filament in the x-ray region. This may indicate that the subcluster is moving toward a central condensation of faint galaxies in the Coma cluster and a possible merger with it. __________ Translated from Astrofizika, Vol. 50, No. 3, pp. 355–368 (August 2007).     

Influence of Neutron Star Parameters on Evolutions of Different Types of Pulsar

Influences of the mass, moment of inertia, rotation, absence of stability in the atmosphere and some other parameters of neutron stars on the evolution of pulsars are examined. It is shown that the locations and evolutions of soft gamma repeaters, anomalous X-ray pulsars and other types of pulsar on the period versus period derivative diagram can be explained adopting values of B < 10¹⁴ G for these objects if they have smaller mass (e.g. about 0.5 Solar mass) compared to the conventionally adopted values of mass. This approach gives the possibility to explain many properties of different types of pulsar.     

淮河洪水的可公度性分析

分析了上两个世纪发生在淮河的洪水事件的可公度性，根据其可公度值及其黄金分割点指出1991年与2003年淮河洪水的不可避免，最后讨论了可公度性的局限及淮河洪水可公度值的可能机制。     

基于STK的寿命末期GEO卫星轨道演化分析

地球同步轨道上的GEO卫星接近寿命末期时,星上的有效载荷和电子元器件等仍能正常应用,此时如果只做东西方向的位置保持,可以大幅度延长卫星的在轨工作寿命。简要介绍了引起GEO卫星轨道变化的主要摄动力,利用STK软件分析寿命末期GEO卫星的运动规律,并给出这类GEO卫星轨道演化的仿真分析流程,用以指导寿命末期GEO卫星的开发应用工作。     

On the application of optimization methods to the determination of members of families of periodic solutions

The techniques used for the numerical computation of families of periodic orbits of dynamical systems rely on predictor-corrector algorithms. These algorithms usually depend on the solution of systems of approximate equations constructed from the periodicity conditions of these orbits. In this contribution we transform the root finding procedure to an optimization one which is applied on an objective function based on the exact periodicity conditions. Thus, the determination of periodic solutions and families of such orbits can be accomplished through unconstrained optimization. In this paper we apply and compare some well-known minimization methods for the solution of this problem. The obtained results are promising. This revised version was published online in July 2006 with corrections to the Cover Date.