基于CAPS,BDS和GPS的组合卫星定位精度分析

随着GPS,GLONASS,Galileo和BDS等全球卫星定位系统的建设和完善,同时采用两个或两个以上定位系统信号进行多系统组合定位成为导航领域研究的热点。相比传统的单系统定位,多系统组合具有更好的定位、测速、授时性能以及更强的环境适应性。通过CAPS,BDS和GPS三个系统的静态单点联合定位解算,实现了转发式定位系统与直发式定位系统的联合定位,验证了中国区域定位系统参与多系统全球导航卫星系统定位的可行性,并分析了组合定位的性能与定位精度。分析表明,中国区域定位系统参与多系统联合定位解算是完全可行的,单点定位精度优于3 m,且还有提高的空间。中国区域定位系统的加入,丰富了全球导航卫星系统的选择,对提高全球导航卫星系统联合定位的多样性,改善联合定位性能具有研究意义及应用价值。     

GPS系统时间及其与其他时间的关系

指出不同授时规范对“GPS系统时间”定义、解释的差异,给出比较清楚和综合的“GPS系统时间”理解,这会有益于北斗系统和GPS系统组合PNT（定位、导航、授时）应用标准化。     

基于GPS和RFID的城市车辆定位系统的设计

详细阐述了城市车辆导航定位技术的发展现状,深入分析了城市车辆导航定位的特点和需求,在此基础上利用嵌入式开发平台设计实现了基于GPS和RFID(无线射频识别)的车载定位系统,系统主要由GPS模块、RFID模块、GPRS(general packet radio service,通用分组无线服务)模块等部分组成。该系统通过接收GPS数据和RFID数据,依托ARM平台进行分析处理,分析处理的结果通过GPRS模块发送到监控中心以实现对车辆的监控与导航。该系统具有实时性好、可靠性高、功耗体积小等显著特点,能够满足现代城市车辆的导航与定位需要。     

嵌入式GPS/DR车载组合导航系统EKF算法软件设计

介绍一种嵌入式GPS／DR（全球定位系统／航位推算）车载组合导航（它通过GPS与DR的优势互补,提高了车辆导航系统定位数据的可靠性）的EKF（扩展卡尔曼滤波）算法软件设计方法。采用统计学原理剔除导航数据的粗差点,用扩展卡尔曼滤波进行导航参数的实时求解,采用EKF算法的GPS／DR组合导航系统有利于导航信息的稳定性、可靠性和实时性。     

GNSS系统时间偏差的确定及其对定位结果的影响

由于GNSS各个导航系统都有独立的系统时间,在GNSS多模导航定位中需要对各导航系统之间的系统时差进行处理。以GPS／GLONASS双模导航为例,讨论了系统时差的解决方法以及系统时差对定位结果的影响。实验结果表明,在多模导航定位中考虑系统时差可以有效地提高定位结果的准确性,改善定位结果的精度。     

Loran-C系统的技术改造与发展方向

简要介绍了近两年来美国和北欧Loran-C系统的研究和技术改造,以及未来数年内的发展方向政策,美国制订了的改造计划,对Loran-C系统及设备进行结构性调整和更新改造,同时对采用新技术后的Loran-C系统的性能和长期需求作出测试与评估,北欧Loran-C系统的研究重心是如何将陆基和空基系统有效地结合起来,Loran-C系统的作为和潜在应用还有于进一步的研究和探索。     

Loran—C和GPS国际时间比对的长期结果比较

根据1990－1994年上海天台（SO）和世界上一些时间中心（国际计量局（BIPM）时间部、美国海军天台（USNO））的时间公报公布的数据，对两种时间传递技术（Loran-C和GPS）确定的国际时间同步的长期结果进行了比较分析。SO时间实验室得到如下一些结果：1、1990－1992年，由Loran-C时间传递技术确定的结果表明：系统差约为600ns，不确定度约为90ns(1σ），准确度估计优于1μs。2、1993－1994年，由GPS时间传递技术确定的结果表明：系统差优于30ns，不确定度约为15ns(1σ），准确度估计优于100ns。这些比较结果充分说明了GPS时间传递技术在国际高水平时间同步的中必须有广泛的应用。     

导航卫星精密定轨与时间同步技术进展

全球卫星导航系统(Global Navigation Satellite System, GNSS)通过播发卫星钟差和精密轨道信息实现时间和空间基准信息向导航用户的传递.随着高精度原子钟等导航卫星载荷、星间链路等天基/地基监测手段以及数据处理方法等技术的不断更新,卫星轨道和钟差产品的精度和实时性也逐步提升. 2018年12月,北斗三号卫星导航系统正式开通,为"一带一路"国家提供实时高精度、高可靠的基本导航定位服务.综述了北斗导航系统从北斗二号区域系统到北斗三号全球系统精密定轨与时间同步处理面临的困难和挑战,针对上述问题,阐述了北斗运行控制系统的解决途径和实现指标.与GPS等其他GNSS系统进行比较,分析了不同导航系统技术特点.最后展望了精密定轨与时间同步技术未来的发展路线图,为更高精度的GNSS导航定位授时服务提供参考.     

GPS 导航电文中时间参数的变化特点

GPS导航电包含有GPS卫星的位置参数和时间参数,是定位,定时用户都必须使用的,随着GPS的改进,导航电民有所变,GPS导航电中时间参数的变化特点及SA对卫星钟的影响是这里着重讨论的内容。     

利用卫星电视系统进行导航的基准站配置

在导航系统中,基准站配置的优劣直接关系到定位的精度及系统的可用性,对利用卫星电视系统进行导航可能采用的几种基准站配置进行了讨论,并对具体问题进行了分析计算,分析认为解决好基准站配置,合理地组合导航系统,可有效地提高定位的精度及系统的可用性。     

Production and processing of silicates in laboratory and in space

Since their formation in the outflows of evolved stars, materials suffer in space deep chemical and physical modifications. Most abundant elements (C, N, O, Mg, Si, S and Fe) are present in dust as refractory chemical species. Among them silicates are one of the main constituents. Spectroscopic observations in various astronomical environments have shown that magnesium rich silicates are present both in amorphous and in crystalline form. An accurate interpretation of these observations requires studies on the formation of silicate dust in the atmospheres of giant stars and their evolution in the interstellar medium until their inclusion in protoplanetary disks.Many theoretical works have described the chemical and physical evolution of solids in space and their link to observable optical properties. Laboratory studies of cosmic dust analogues are needed to investigate these processes experimentally.In this work, experiments aimed at simulating the formation of silicates in space are presented. In particular, the laser ablation technique is used to produce amorphous silicates with various Si-Mg-Fe content. The analysis of their thermal evolution is presented.     

Gemini observations of disks and jets in young stellar objects and in active galaxies

We present first results from the Near-infrared Integral Field Spectrograph (NIFS) located at Gemini North. For the active galaxies Cygnus A and Perseus A we observe rotationally-supported accretion disks and adduce the existence of massive central black holes and estimate their masses. In Cygnus A we also see remarkable high-excitation ionization cones dominated by photoionization from the central engine. In the T-Tauri stars HV Tau C and DG Tau we see highly-collimated bipolar outflows in the [Fe II] λ 1.644 micron line, surrounded by a slower molecular bipolar outflow seen in the H₂ lines, in accordance with the model advocated by Pyo, T.-S., et al., Astrophys. J. 570, 724 (2002).     

Supernovae in isolated galaxies, in pairs and in groups of galaxies

In order to investigate the influence of environment on supernova (SN) production, we have performed a statistical investigation of the SNe discovered in isolated galaxies, in pairs and in groups of galaxies. 22 SNe in 18 isolated galaxies, 48 SNe in 40 galaxy members of 37 pairs and 211 SNe in 170 galaxy members of 116 groups have been selected and studied.
We found that the radial distributions of core-collapse SNe in galaxies located in different environments are similar, and consistent with those reported by Bartunov, Makarova & Tsvetkov . SNe discovered in pairs do not favour a particular direction with respect to the companion galaxy. Also, the azimuthal distributions inside the host members of galaxy groups are consistent with being isotropics. The fact that SNe are more frequent in the brighter components of the pairs and groups is expected from the dependence of the SN rates on the galaxy luminosity.
There is an indication that the SN rate is higher in galaxy pairs compared with that in groups. This can be related to the enhanced star formation rate in strongly interacting systems.
It is concluded that, with the possible exception of strongly interacting systems, the parent galaxy environment has no direct influence on SN production.     

The abundance of helium in prominences and in the chromosphere

The abundance of helium relative to hydrogen is spectroscopically determined in prominences and in the chromosphere by using 1952, 1958, 1962 and 1966 eclipse data. Care is taken in the intensity calibration of emission lines, the self-absorption, and the departure from local thermodynamic equilibrium. We find from the line profiles and intensities of prominences and the chromosphere that the neutral helium lines are emitted in the metal-hydrogen emitting region where the kinetic temperature is low enough, 6000 8000 K, so that only the ionization due to UV radiation from the corona can explain the intensity of neutral helium emission. Also we find that the intensity ratio of Hei 3888.65 to H₈ 3889.05 increases towards the upper boundaries of prominences and of the chromosphere and that it approaches to a universal limiting value, both in various prominences or in the chromosphere, where it is considered that the ionization of neutral helium and hydrogen is nearly complete. From these facts the helium to hydrogen number ratio is found to be 6.5 ± 1.5%.A new schematic model of the chromosphere is presented where spicules have no hot region of emitting neutral helium lines. Here it is suggested that the kinetic temperature of spicules, 6000 8000 K, would be primarily determined by the radiation temperature of the corona and the transition region beyond the Lyman continuum of hydrogen which happens to be around those temperatures.     

Tidal and rotational distortions in figures of Pluto and Charon

The supposition is, the tidal and rotational distortions should be fully responsible for the Pluto's and Charon's figure parameters. The mean polar and equatorial flattenings have been estimated about 10^–3, the second sectorial Stokes parameters about 9 × 10^–5, the differences between equatorial principal moments of inertia about 6 × 10³⁰ kg m² (Pluto) and 2 × 10²⁹ kg m² (Charon).     

Characteristics of convection and overshooting in RGB and AGB stars

Based on the turbulent convection model (TCM) of Li & Yang, we have studied the characteristics of turbulent convection in the envelopes of 2 and 5M⊙ stars at the red giant branch and asymptotic giant branch phases. The TCM has been successfully applied over the entire convective envelopes, including the convective unstable zone and the overshooting regions. We find that the convective motions become progressively stronger when the stellar models are located farther up along the Hayashi line. In the convect...     

Relativistic beaming effects in the spectra of cores and hotspots in radio galaxies and quasars

We present the results of multiwavelength observations of cores and hotspots, at L , C , X and U bands with the Very Large Array, of a matched sample of radio galaxies and quasars selected from the Molonglo Reference Catalogue . We use these observations to determine the spectra of cores and hotspots, and test the unified scheme for radio galaxies and quasars. Radio cores have been detected at all wavelengths in all of the quasars in our sample, whereas only ∼50 per cent of the galaxies have cores detected in at least one of the wavelengths . The degree of core prominence in this sample is consistent with the unified scheme for radio galaxies and quasars. A comparison of the distributions of the two-point spectral index of the cores in our sample of lobe-dominated quasars, with the distributions in a matched sample of core-dominated quasars, shows that the distributions for these two classes are significantly different, and this is consistent with the expectations of the unified scheme. The difference in the spectral indices of the two hotspots on opposite sides is also significantly larger for quasars than for radio galaxies, as is expected in the unified scheme. We also investigate the relationship between the spectral index of the hotspots and the redshift or luminosity for our sample of sources.     

Electrolysis in space and fate of Phaethon

A new process of the energy accumulation in icy bodies (e.g., planetary satellites, cometary nuclei) is advanced which is applicable for space conditions: namely, the volumetric electrolysis of the ice containing foreign inclusions. The electrolysis takes place when the electric current, generated by virtue of the body's movement in the external magnetic field (planetary magnetospheres, the solar wind field, etc.) flows through the body.The cosmogonical concept which treats the Sun-Jupiter system as a limiting case of a close binary star, together with the known data on mass, composition and space distribution of asteroids, allows one to assume the initial existence between Mars and Jupiter of a Moon-like planet enriched with ices and allied by its parameters to the Galilean satellites (mainly Ganymede and Callisto). If this planet was affected by the ancient solar wind with during 10⁹ yr, it could have accumulated the energy sufficient for its explosion.The process considered seems able to explain, from a unified point of view, a large number of phenomena — such as the burst activity of comets, a considerable hydrogen excess in their tails, a noticeable long-period comet perihelia orientation toward the solar apex, the existence of asteroidal families and the separation of asteroids by their chemical composition into two main groups, the Tunguska event, etc.