Interannual variability of low-degree gravitational change, 1980–2002     

J.L. Chen  C.R. Wilson  B.D. Tapley 《Journal of Geodesy》2005,78(9):535-543

Time variations in the Earths gravity field at periods longer than 1 year, for degree-two spherical harmonics, C₂₁, S₂₁, and C₂₀, are estimated from accurately measured Earth rotational variations. These are compared with predictions of atmospheric, oceanic, and hydrologic models, and with independent satellite laser ranging (SLR) results. There is remarkably good agreement between Earth rotation and model predictions of C₂₁ and S₂₁ over a 22-year period. After decadal signals are removed, Earth-rotation-derived interannual C₂₀ variations are dominated by a strong oscillation of period about 5.6 years, probably due to uncertainties in wind and ocean current estimates. The model-predicted C₂₀ agrees reasonably well with SLR observations during the 22-year period, with the exception of the recent anomaly since 1997/1998.  相似文献   

Scale factor calibration of a superconducting gravimeter at Esashi Station, Japan, using absolute gravity measurements     

Y. Tamura  T. Sato  Y. Fukuda  T. Higashi 《Journal of Geodesy》2005,78(7-8):481-488

The scale factor of a superconducting gravimeter (SG) at the Esashi Earth Tides Station, Japan, was revised by repeating co-located absolute gravity measurements with an FG5 gravimeter. Although the calibration results from the absolute gravimeter (AG) show an apparent secular change in the scale factor of the SG (0.4% for the period 1993–2002), the relative scale factors, which are determined by tidal analysis with the response method, indicate that it has changed by no more than 0.01% during the above period. If the mean scale factor over the 10 years is adopted, a value of –56.082±0.029 Gal/V (1 Gal =10^–8 m s^–2) is obtained, which is about 0.4% smaller than that used in the global geodynamics project (GGP) database. Based on this newly determined scale factor, the tidal gravity factors at Esashi have been re-estimated. The observed tidal factors, corrected for the ocean tide effects with recent models, indicate that the theoretical gravity factors for an inelastic Earth model are more consistent with the observations than are those for an elastic model.  相似文献   

浅谈固体地球科学与地球系统科学   总被引：5，自引：0，他引：5  

郭正堂  吴海斌 《地球科学进展》2004,19(5):699-705

地球科学在20世纪的诸多进展中,对后来科学发展具有深远影响的基本认识之一是地球演化的行为具有整体性,其不同的圈层确实通过多种途径相互作用,且人类活动已成为地球演化的重要营力之一。这些认识导致地球系统科学思想的产生和发展,并使不同圈层相互作用的过程和机理、人与环境的相互作用研究成为21世纪基础科学研究的前沿。地球系统科学强调地球不同圈层、不同单元相互作用的整体性和关联性,因而科学研究必须从"整体地球系统"的视野出发,但研究过程又必须从关键区域入手。我国是地球系统科学研究的关键地区之一,未来研究应立足地域优势和特色,攻克全球性重大科学问题,解决社会对地球科学的知识需求。  相似文献   

Formation of terrestrial planets in a dissipating gas disk with Jupiter and Saturn     

Junko Kominami  Shigeru Ida 《Icarus》2004,167(2):231-243

We have performed N-body simulations on final accretion stage of terrestrial planets, including the eccentricity and inclination damping effect due to tidal interaction with a gas disk. We investigated the dependence on a depletion time scale of the disk, and the effect of secular perturbations by Jupiter and Saturn. In the final stage, terrestrial planets are formed through coagulation of protoplanets of about the size of Mars. They would collide and grow in a decaying gas disk. Kominami and Ida [Icarus 157 (2002) 43-56] showed that it is plausible that Earth-sized, low-eccentricity planets are formed in a mostly depleted gas disk. In this paper, we investigate the formation of planets in a decaying gas disk with various depletion time scales, assuming disk surface density of gas component decays exponentially with time scale of τ_gas. Fifteen protoplanets with are initially distributed in the terrestrial planet regions. We found that Earth-sized planets with low eccentricities are formed, independent of initial gas surface density, when the condition (τ_cross+τ_growth)/2?τ_gas?τ_cross is satisfied, where τ_cross is the time scale for initial protoplanets to start orbit crossing in a gas-free case and τ_growth is the time scale for Earth-sized planets to accrete during the orbit crossing stage. In the cases satisfying the above condition, the final masses and eccentricities of the largest planets are consistent with those of Earth and Venus. However, four or five protoplanets with the initial mass remain. In the final stage of terrestrial planetary formation, it is likely that Jupiter and Saturn have already been formed. When Jupiter and Saturn are included, their secular perturbations pump up eccentricities of protoplanets and tend to reduce the number of final planets in the terrestrial planet regions. However, we found that the reduction is not significant. The perturbations also shorten τ_cross. If the eccentricities of Jupiter and Saturn are comparable to or larger than present values (∼0.05), τ_cross become too short to satisfy the above condition. As a result, eccentricities of the planets cannot be damped to the observed value of Earth and Venus. Hence, for the formation of terrestrial planets, it is preferable that the secular perturbations from Jupiter and Saturn do not have significant effect upon the evolution. Such situation may be reproduced by Jupiter and Saturn not being fully grown, or their eccentricities being smaller than the present values during the terrestrial planets' formation. However, in such cases, we need some other mechanism to eliminate the problem that numerous Mars-sized planets remain uncollided.  相似文献   

Effects of the number of stations and time resolution on derivation     

Odim Mendes  Jr.  Aracy Mendes da Costa  Fernando Celso Perin Bertoni 《Journal of Atmospheric and Solar》2006,68(18):2127-2137

For at least 30 years now it has been well known that the Dst index can be modelled using the solar wind as input. Since then, many attempts have been made to improve the predictability of Dst using different approaches. These attempts are useful, for instance, to understand which features of the solar wind–magnetosphere interactions are most important in producing magnetospheric activity and how the Dst index would improve the space weather forecast. The Dst index is by far the most reliable and simple indication that a magnetic storm is in progress. In this work, the effect of using more than four magnetic stations and shorter time intervals than the hourly averages used in Sugiura's procedures is evaluated. The discussion is based on the results presented by Burton in 1975 and Feldstein in 1984 considering 4 or 12 magnetic stations and time averages of 2.5 min for a magnetic disturbed period that occurred from February 7–28, 1967, including two geomagnetic storms. The analysis has shown that the global representation of a magnetic storm by the standard Dst (Sugiura) is well preserved either using 4, 6, 12 magnetic stations or using 1 h, 2.5 min 1 min averages. A brief review of the current understanding of Dst has been included to support the discussions. The analysis performed has shown that a more refined Dst index (time and number of stations>4) would be useful to investigate the intrinsic processes and the different current systems involved in the ring current development during magnetic storms; the standard Dst, as it is conceived, is quite adequate to monitor geomagnetic storms and identify their overall features; concerning the magnetic stations normally considered, the inclusion of higher magnetic latitude stations (>35) may underestimate the observed Dst.  相似文献   

Numerical theory of rotation of the deformable Earth with the two-layer fluid core. Part 1: Mathematical model     

G. A. Krasinsky 《Celestial Mechanics and Dynamical Astronomy》2006,96(3-4):169-217

Improved differential equations of the rotation of the deformable Earth with the two-layer fluid core are developed. The equations describe both the precession-nutational motion and the axial rotation (i.e. variations of the Universal Time UT). Poincaré’s method of modeling the dynamical effects of the fluid core, and Sasao’s approach for calculating the tidal interaction between the core and mantle in terms of the dynamical Love number are generalized for the case of the two-layer fluid core. Some important perturbations ignored in the currently adopted theory of the Earth’s rotation are considered. In particular, these are the perturbing torques induced by redistribution of the density within the Earth due to the tidal deformations of the Earth and its core (including the effects of the dissipative cross interaction of the lunar tides with the Sun and the solar tides with the Moon). Perturbations of this kind could not be accounted for in the adopted Nutation IAU 2000, in which the tidal variations of the moments of inertia of the mantle and core are the only body tide effects taken into consideration. The equations explicitly depend on the three tidal phase lags δ, δ _c, δ _i responsible for dissipation of energy in the Earth as a whole, and in its external and inner cores, respectively. Apart from the tidal effects, the differential equations account for the non-tidal interaction between the mantle and external core near their boundary. The equations are presented in a simple close form suitable for numerical integration. Such integration has been carried out with subsequent fitting the constructed numerical theory to the VLBI-based Celestial Pole positions and variations of UT for the time span 1984–2005. Details of the fitting are given in the second part of this work presented as a separate paper (Krasinsky and Vasilyev 2006) hereafter referred to as Paper 2. The resulting Weighted Root Mean Square (WRMS) errors of the residuals dθ, sin θd for the angles of nutation θ and precession are 0.136 mas and 0.129 mas, respectively. They are significantly less than the corresponding values 0.172 and 0.165 mas for IAU 2000 theory. The WRMS error of the UT residuals is 18 ms.  相似文献   

大型工程中的WMS数据获取与集成应用方法     

韩元利  刘一平  王汉东  朱庆 《武汉大学学报(信息科学版)》2012,37(6):741-745

面向大型土木工程设计,提出了一种运用WMS共享空间数据源并实现高效应用集成的工程设计应用技术体系。首先,直接针对WMS数据服务器定向开发数据获取应用,通过高效并行多线程实现空间数据的分块网络传输,同时结合本地缓存机制与网络共享,实现了一种双轨存储访问机制;其次,基于独立的应用下载与嵌入的实时线程分配,实现了远程数据的本地化模拟应用环境与分布式共享协同;再次,针对WMS数据的应用,实现了空间数据向工程数据的高精度转换与工程制图出图体系,开发了统一的全球三维可视化平台,用于直观地综合表达各种WMS数据源。  相似文献   

风云三号卫星微波成像仪在轨性能稳定性分析     

乔木  杨虎  何嘉恺  吕利清 《遥感学报》2012,16(6):1246-1261

利用地球冷目标观测亮温的稳定性和遥感数据统计直方图方法,是评价微波成像仪等类似微波成像辐射计在轨性能稳定性的有效方法。在此基础上,本文用2011年2月—7月风云三号02星微波成像仪在轨观测的亮温数据,对微波成像仪在轨运行的性能稳定性进行了分析。结果表明:风云三号02星微波成像仪在轨性能稳定,所有通道最低亮温参考值波动范围不超过1.8K。  相似文献   

全球模式NCAR CESM和CAS ESM对亚洲东部夏季气候的模拟性能评估:气候平均态和降水日变化分析     

李星雨  毕训强  张贺 《气候与环境研究》2018,23(6):645-656

主要评估了美国国家大气研究中心的NCAR CESM（Community Earth System Model,NCAR）和中国科学院的CAS ESM（Earth System Model,Chinese Academy of Sciences）两个地球系统模式对亚洲东部夏季气候态的模拟性能。使用NCAR CESM和CAS ESM各两种不同的水平分辨率,一共进行了4组长达19年（1998~2016年）的数值积分试验,并通过对2 m气温、降水强度和降水日变化等的分析,比较了这两个模式在亚洲东部的模拟性能。结果表明,CAS ESM和NCAR CESM均能模拟出夏季2 m气温和降水强度的大尺度分布特征,但整体上模拟得到的地表面气温偏暖、降水强度偏弱。对于降水日变化而言,观测的日降水峰值在陆地上主要发生在下午到傍晚时段,在海洋上则出现在午夜到凌晨时段。两组低分辨率试验模拟的陆地降水峰值出现过早,且无法模拟出四川盆地的夜间降水峰值和部分海洋地区凌晨或上午的降水峰值。提高分辨率对模式的模拟性能有显著的提升作用。高分辨率下,NCAR CESM和CAS ESM对陆地和海洋的降水日变化模拟性能都明显提高。对降水日变化的定量化分析表明,高分辨率CAS ESM模式对整个亚洲东部降水日变化的模拟最优。目前模式对海陆风的模拟还不太理想,未来要进一步提高模式模拟性能,需要重点完善与气温、降水过程相关的物理参数化方案。  相似文献   

2009年6月九江一次典型雷击事故原因分析     

黄中根  齐移民 《气象与减灾研究》2010,33(3):69-72

根据2009年6月江西省九江一次雷击事故现场的勘察结果,利用雷电监测数据和剩磁检测数据对雷电流大小进行了对比分析,认为造成雷击事故的可能原因有三方面,分别是电源SPD的保护级别不够、SPD的容量太小、接地引下线过长和截面积太小。最后,提出了相应的整改建议。  相似文献