GPS-only gravity field recovery with GOCE,CHAMP, and GRACE

Gravity missions such as the Gravity field and steady-state Ocean Circulation Explorer (GOCE) are equipped with onboard Global Positioning System (GPS) receivers for precise orbit determination (POD), instrument time-tagging, and the extraction of the long wavelength part of the Earth’s gravity field. The very low orbital altitude of the GOCE satellite and the availability of dense 1 s GPS tracking data are ideal characteristics to exploit the contribution of GPS high-low Satellite-to-Satellite Tracking (hl-SST) to gravity field determination. We present gravity field solutions based on about 8 months of GOCE GPS hl-SST data from 2009 and compare the results with those obtained from the CHAllenging Minisatellite Payload (CHAMP) and Gravity Recovery And Climate Experiment (GRACE) missions. The very low orbital altitude of GOCE significantly improves gravity field recovery from GPS hl-SST data above degree 20, but not for the degrees below 20, where the quality of the spherical harmonic coefficients remains essentially unchanged. Despite the limited time span of GOCE data used, the gravity field of the Earth can be resolved up to about degree 115 using GPS data only. Empirically determined phase center variations (PCVs) of the GOCE onboard GPS helix antenna are, however, mandatory to achieve this performance.     

Impact of covariance information of kinematic positions on orbit reconstruction and gravity field recovery

Gravity missions are equipped with onboard Global Positioning System (GPS) receivers for precise orbit determination (POD) and for the extraction of the long wavelength part of the Earth’s gravity field. As positions of low Earth orbiters (LEOs) may be determined from GPS measurements at each observation epoch by geometric means only, it is attractive to derive such kinematic positions in a first step and to use them in a second step as pseudo-observations for gravity field determination. The drawback of not directly using the original GPS measurements is, however, that kinematic positions are correlated due to the ambiguities in the GPS carrier phase observations, which in principle requires covariance information be taken into account. We use GRACE data to show that dynamic or reduced-dynamic orbit parameters are not optimally reconstructed from kinematic positions when only taking epoch-wise covariance information into account, but that essentially the same orbit quality can be achieved as when directly using the GPS measurements, if correlations in time are taken into account over sufficiently long intervals. For orbit reconstruction covariances have to be considered up to one revolution period to avoid ambiguity-induced variations of kinematic positions being erroneously interpreted as orbital variations. For gravity field recovery the advantage is, however, not very pronounced.     

火星卫星的冻结轨道研究

冻结轨道是一种稳定的轨道,地球、火星、月球的卫星因引力场的南北不对称,都存在冻结轨道.由于主星体引力场的不同,它们卫星的冻结轨道也有不同的特性.地球卫星的冻结执道的偏心率非常小,对卫星遥感非常有利,国内外已有相当多的近地遥感卫星采用这种轨道.月球卫星的冻结轨道偏心率随轨道倾角的不同有很大的变化,对月球卫星冻结轨道的研究...     

捕获轨迹系统并联机构地面标定方法

捕获轨迹系统（CTS）是一种先进的预测外挂物投放轨迹的试验系统，普遍采用六自由度（6-DoF）串联机构作为其运动机构，串联机构因惯性力大和关节累积误差大使其定位精准度不足。相比串联机构，并联机构具有惯性力小和关节误差不累积等优点。采用6-PTRT并联机构作为CTS试验系统的六自由度运动机构，在空间受限的风洞环境中对CTS并联机构进行地面标定：提出动平台位姿的测量和计算方法，建立包含直线驱动平台安装夹角修正的标定模型，并基于非线性最小二乘法辨识结构参数。辨识后CTS并联机构的位移定位准度优于0.1 mm，姿态定位准度优于0.05°，最后以CTS并联机构和常规攻角机构进行8#标模的对比风洞试验。风洞试验结果表明，CTS并联机构的风载定位准度满足测力试验精准度要求。     

速率转台低角速率校准方法探讨

主要描述速率转台低角速率的一种校准方法,并对该方法进行分析探讨.     

Needs and Tools for Future Gravity Measuring Missions

This paper compares the requirements that can be expected of gravity measuring missions with respect to the status of the instrumentation and satellite technologies. The error sources of gravity gradiometry and satellite-to-satellite tracking are analysed and the elements limiting the accuracy are identified. Proposed and approved future missions that will fly technologies of interest for gravity sensing are recalled. Areas of technical development of interest are reviewed. The article finishes with two possible conceptual missions presented as examples and with a chapter of conclusions. This revised version was published online in August 2006 with corrections to the Cover Date.     

井田制与租佃制的比较分析

井田制内含耕地资源所有权和经营权分离,租佃制则是耕地资源所有权与经营权分离的普遍化,二者都以耕地资源私有制和资源有偿利用为基础。给我们的启示是:公有资源按照所有权与经营权相分离的模式必产生公有制经济形式多样。     

Seismology of Prominence-Fine structures: Observations and Theory

Prominence seismology is a rapidly developing topic which seeks to infer the internal structure and properties of solar prominences from the study of its oscillations. Two-dimensional high-resolution observations suggest that filaments can be considered as made by small scale fibrils, having a cool region, stacked one after another in the vertical and horizontal directions. An extense observational background about oscillations in filaments has been gathered during the last 20 years and these observations point out that fibrils or groups of fibrils can oscillate independently. From the theoretical point of view, small amplitude oscillations in single and multifibril configurations have been studied as a first step to explain observational features.     

用一种非线性k-ε模型计算突扩台阶后的流动

对一种新的非线性k-ε模型的无量纲系数进行了重新拟合.用新的系数计算了槽道流动、方截面管流和等应变率,平均流场无旋流动的正应力分布.计算结果与实验资料符合很好.将该模型并入常规的k-ε模型的计算程序中,并对突扩台阶后的湍流流动进行了数值计算,同线性k-ε模型的计算结果和实验结果进行了比较.结果表明,这种非线性k-ε模型同线性模型相比有较大的改进,同已有的其它非线性模型相比,也有一定的优点.     

Summary of the workshop on gamma-ray burst afterglows at the 34th COSPAR meeting

A summary is given of the presentations at the COSPAR workshop on γ-ray bursts with some personal commentary on the contributions, the SN/GRB connection, and on the role of magnetic fields in γ-ray bursts and their afterglows. Of special interest were the accumulated arguments for strong collimation and associated reduction in the total required energy for γ-ray bursts. Significant discussion was also devoted to the issues associated with iron and metal lines in X-ray spectra. It is important to note that some of the afterglows seem to require ambient densities 1 g cm⁻³, rather incompatible with a massive star environment. Of associated difficulty is the fact that few, if any, afterglows seem consistent with the r⁻² wind expected for a massive star model. There are reasons to think that if γ-ray bursts are associated with supernovae they are of Type Ic. This suggests that any wind present might be rich in carbon and oxygen, not hydrogen or helium. If γ-ray bursts are narrowly collimated, then the burst is only probing a small portion of any wind, perhaps just that time-dependent and isotropic structure directly along the rotation axis. The characteristics of “hypernovae” may be the result of orientation effects in a mildly inhomogeneous set of progenitors, rather than requiring an excessive total energy or luminosity. The recent event GRB 021004 provided a rich photometric and spectroscopic record and perhaps the most direct evidence yet for the association of a specific γ-ray burst with a massive star progenitor. If the magnetic field plays a significant role in launching a relativistic γ-ray burst jet from within a collapsing star, then the magnetic field may also play a role in the propagation, collimation, and stability of that jet within and beyond the star. The magneto-rotational instability (MRI) can operate under conditions of moderate rotation. This means that the MRI will be at work generating strong fields exponentially rapidly even as the disk of material begins to form and makes a transition from a non-Keplerian to quasi-Keplerian flow in the collapsar and related models.