共查询到20条相似文献，搜索用时 137 毫秒
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《天文研究与技术》2015,(4)
FAST望远镜馈源舱通过6根钢索悬浮于空中,在运行过程中其倾角连续变化,存在发生倾覆的风险。通过舱索系统的静力学理论分析和模型试验对FAST馈源舱的最大倾覆角进行了研究。基于舱倾角最大的优化原则和舱-索系统静力平衡,对索力和姿态角的限定等约束条件,建立了求解舱最大倾角(倾覆角)的目标优化函数,利用牛顿迭代法解得了舱在其运行轨迹面(焦面)的倾覆角,同时研究了重心改变对倾覆角的影响。通过舱索系统3 m缩尺模型对理论分析结果进行了验证,得到了模型舱在给定位置的倾覆角,试验结果与理论计算结果比较吻合。最后分析了馈源舱原型在整个焦面上的倾覆角,结果表明馈源舱在实际工作过程中是安全的,不会发生倾覆。 相似文献
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伪距测量中的时标偏差影响分析 总被引：3，自引：0，他引：3
伪距是卫星导航系统的基本观测量,是实现导航定位、精密定轨和精确授时的基础。基于伪距、钟差和时标偏差的概念与定义,讨论了时标偏差对卫星伪距测量的影响特性;在此基础上,给出了利用伪距O-C(观测值与计算值之差)进行时标偏差解算的计算模型;理论分析表明:时标偏差影响主要体现在伪距变率项;对于MEO卫星,时标偏差影响不仅会使真实的O-C曲线斜率变大、曲线变长,而且会使多个弧段O-C曲线呈现锯齿状,表现为每个弧段解算的参数不能用于跨弧段预报。最后,利用北斗试验系统MEO卫星实测数据进行了验证分析,试验结果表明:采用实测数据计算的时标偏差精度约在0.02s左右,不同弧段解算结果比较稳定,并且扣除时标偏差后的O-C计算结果也与理论结果具有较好的一致性,从而验证了本文时标偏差理论分析和计算模型的正确性。 相似文献
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《中国科学院上海天文台年刊》2016,(0)
介绍了在广义相对论框架下建立的微米级卫星激光测距时延模型。为考察新模型对于参数化后牛顿系数β和γ解算精度的影响,将该模型用于定轨软件Utopia对Ajisai,Lageos 1,Lageos 2,Etalon 1四颗卫星的模拟观测资料进行批处理,并假设大气、固体潮等观测模型的效应以及动力学模型的误差已精确扣除。结果表明,在当前的仿真条件下采用微米级时延模型解算的参数化后牛顿系数解算精度比采用现有的标准时延模型的解算精度高2个量级。 相似文献
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500 m球面射电望远镜(The Five-hundred-meter Aperture Spherical radio Telescope, FAST)馈源舱位置和姿态测量精度直接影响望远镜接收机的对准精度.为了提高馈源舱位姿精度,提出姿态卡尔曼滤波算法,采用北斗导航系统的多天线技术解算馈源舱姿态,将它与捷联惯导解算的馈源舱姿态对比,两者的差值作为姿态卡尔曼滤波的量测量.为了降低北斗导航系统解算姿态的复杂度,采用了罗德里格矩阵解算方法.以望远镜跟踪观测模式时,北斗导航系统和捷联惯导解算的实际导航结果作为测试数据,测试结果表明采用姿态卡尔曼滤波的组合导航结果精度优于传统卡尔曼滤波的组合导航结果,尤其在航向角和yf轴的位置精度上. 相似文献
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在有2个探测器的深空探测中,利用同波束VLBI技术可解算高精度的差分相时延,进而同时提高2个探测器的测定轨精度。但是,差分相时延的解算条件严格,差分相位抖动较大时直接影响解算的成功率。针对这一问题,利用SELENE两颗小卫星Rstar和Vstar的4个测站长达1年的同波束VLBI观测数据,统计得出了差分相位抖动与其对应的角距离的关系模型。该模型的建立,既有利于提高同波束VLBI差分相时延的解算成功率,又对行星中性大气和电离层掩星观测研究具有重要的参考意义。 相似文献
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原子钟的统计模型及其解算方法是建立原子时基准的重要内容之一。利用Kalman滤波技术模拟原子钟运行过程和预测过程的未来值,以及由此建立起来的原子钟噪声模型和整套解算方法正在逐步完善并不断地得到重视和应用。文章回顾了近10年来国内外在时频领域中应用Kalman滤波技术的概况;简要介绍了原子钟的状态模型及其Kalman滤波算法;在此基础上,详细介绍了自适应Kalman滤波算法的原理、方法以及计算结果。 相似文献
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常英立 《中国科学院上海天文台年刊》2007,(1):172-184
该文介绍了解算直角坐标系下不可压缩Navier．Stokes方程的大型有限差分并行软件包NaSt3DGP。介绍了其采用的区域分解算法、差分格式及计算流程；对并行效率进行了测试，作出了处理器数目和计算效率的关系曲线；把此程序应用到旋转的行星流体动力学中，分别用自检验和互检验的方法证明了修改后程序的可靠性，并且得到了满意的非线性数值模拟结果。 相似文献
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The Unified State Model is a method for expressing orbits using a set of seven elements. The elements consist of a quaternion
and three parameters based on the velocity hodograph. A complete derivation of the original model is given in addition to
two proposed modifications. Both modifications reduce the number of state elements from seven to six by replacing the quaternion
with either modified Rodrigues parameters or the Exponential Map. Numerical simulations comparing the original Unified State
Model, the Unified State Model with modified Rodrigues parameters, and the Unified State Model with Exponential Map, with
the traditional Cartesian coordinates have been carried out. The Unified State Model and its derivatives outperform the Cartesian
coordinates for all orbit cases in terms of accuracy and computational speed, except for highly eccentric perturbed orbits.
The performance of the Unified State Model is exceptionally better for the case of orbits with continuous low-thrust propulsion
with CPU simulation time being an order of magnitude lower than for the simulation using Cartesian coordinates. This makes
the Unified State Model an excellent state propagator for mission optimizations. 相似文献
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Paul David Bristow Joël Vernet Sabine Moehler Andrea Modigliani Florian Kerber Michael R. Rosa 《Experimental Astronomy》2011,31(2-3):131-156
We show how traditional instrument quality control trending can be augmented by the use of a physical instrument model. The ESO VLT archive contains a detailed record of instrument diagnostics and calibration parameters while ESO quality control monitors changes in critical parameters. The physical model allows changes in positions, orientations and other physical properties of a spectrograph to be determined from standard wavelength calibration exposures via an optimisation process that seeks the physical model parameters that best reproduce the calibration features in the data. We introduce physical model parameters to the quality control monitoring. When applying this technique to archived calibration exposures, we find that the results are sensitive to the combination of parameters open to the optimisation process. Therefore we determine the most favourable set of physical parameters to optimise for each arm. We then show correlations between several physical parameters and instrument temperature sensor readings and epoch. In addition we find clear discontinuities in some physical parameter values that correspond to known maintenance events. 相似文献
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G.L. Berge 《Icarus》1972
We present new 6.0 and 21.1 cm interferometric observations of Venus. When combined with our previous 3.12 cm work they provide s self-consistent set of high-resolution observations at three wavelengths covering a range in which the opacity of the Venus atmosphere varies by a factor of 50. Model calculations indicate that a model atmosphere of CO2 in adiabatic equilibrium containing uniformly mixed gaseous absorbers surrounding a dielectric sphere cannot simultaneously and adequately predict the radio interferometric measurements at all wavelengths together with the radar and radio occultation measurements. 相似文献
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Models of the iron Kα fluorescent line and the Compton Shoulder in irradiated accretion disc spectra
We present a full set of model atmosphere equations for the accretion disc around a supermassive black hole irradiated by a hard X-ray lamp of power-law spectral distribution. Model equations allow for multiple Compton scattering of radiation on free electrons, and for large relative photon–electron energy exchange at the time of scattering. We present spectra in specific intensities integrated over the disc surface. Theoretical outgoing intensity spectra show soft X-ray excess below 1 keV, and distinct Kα and Kβ fluorescent lines of iron. We demonstrate the existence of the Compton Shoulder and claim that it can contribute to the asymmetry and equivalent widths of some observed Fe Kα lines in active galactic nuclei. Our models exhibit the effect of limb-brightening in reflected X-rays. 相似文献
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A three-dimensional, time-dependent model of thermospheric dynamics has been used to interpret recent experimental measurements of high altitude winds by rocket-borne and ground-based techniques. The model is global and includes a self-consistent treatment of the non-linear, Coriolis and viscosity terms. The solar u.v. and e.u.v. energy input provides the major energy source for the thermosphere. Solar u.v. and e.u.v. heating appear to be inadequate to explain observed thermospheric temperatures if e.u.v. heating efficiency (ε) lies in the range 0.3 < ε < 0.35. If the recent solar e.u.v. data are correct, then a value of ε between 0.4 and 0.45 would bring fluxes and observed temperatures into agreement. The Heppner (1977) and Volland (1978) models of high-latitude electric field are used to provide sources of both momentum (via ion drag) and energy (via Joule heating). We find that the Heppner Model CO (equivalent to Volland Model 1) is most appropriate for very quiet geomagnetic conditions (Kp ? 2) while Model A (equivalent to Volland Model 2) provides the necessary enhancement at high latitudes for conditions of moderate activity (Kp ～ 4). Even with the addition of a polar electric field, there still appears to be a shortage of high-latitude energy input in that model winds tend to be 10 m s?1 poleward of observed winds under quiet or average geomagnetic conditions. This extra energy cannot be provided by enhancing the polar electric fields since the extra momentum would cause disagreement with the observed high latitude winds. High latitude particulate sources of relatively low energies, ~100 eV, seem the most likely candidates depositing their energy above about 200km. Relatively modest amounts of energy are then required, < 1010W global, to bring the model into agreement with both high- and mid-latitude neutral wind results. 相似文献
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D. Ulusen J.G. Luhmann Y.-J. Ma S. Ledvina T.E. Cravens K. Mandt J.H. Waite J.-E. Wahlund 《Icarus》2010,210(2):867-880
Cassini’s Titan flyby on 16 April, 2005 (T5) is the only encounter when the two main ionizing sources of the moon’s atmosphere, solar radiation and corotating plasma, align almost anti-parallel. In this paper a single-fluid multi-species 3D MHD model of the magnetospheric plasma interaction for T5 conditions is analyzed. Model results are compared to observations to investigate the ionospheric dynamics at Titan as well as to understand the deviations from a typical solar wind interaction, such as Venus’ interaction with the solar wind. Model results suggest that for the T5 interaction configuration, corotating plasma is the dominant driver determining the global interaction features at high altitudes. In the lower ionosphere below ～1500 km altitude – where the control of the ionospheric composition transfers from dynamic to chemical processes – magnetic and thermal pressure gradients oppose each other locally, complicating the ionospheric dynamics. Model results also imply that the nightside ionosphere – produced only by the impact ionization in the model – does not provide enough thermal pressure to balance the incident plasma dynamic pressure. As a result, the induced magnetic barrier penetrates into the ionosphere by plasma convection down to ～1000 km altitude and by magnetic diffusion below this altitude. Moreover, strong horizontal drag forces due to ion-neutral collisions and comparable drag forces estimated from possible neutral winds in the lower ionosphere below ～1400 km altitude oppose over local regions, implying that the Titan interaction must be treated as a 3D problem. Ion and electron densities calculated from the model generally agree with the Cassini Ion Neutral Mass Spectrometer and Langmuir probe measurements; however, there are significant differences between the calculated and measured magnetic fields. We discuss possible explanations for the discrepancy in the magnetic field predictions. 相似文献
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望远镜静态指向模型的基本参数 总被引：5，自引：0，他引：5
对地平式望远镜静态指出模型的基本参数进行了讨论，给出了一种参数较少，模型稳定的望远镜修正模型，与常用的球谐函修正模型相比较，基本参数模型具有对观测资料分布不敏感，模型的系随资料分布变化较小和修正精度较高优点，并且其残差序列服从正态分布，基本上能够满足高精度定轨的需要。 相似文献
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G. P. Horedt 《Astrophysics and Space Science》1972,15(1):129-136
We describe two possibilities for the formation of a star by transition of molecular hydrogen from gaseous to the liquid phase in the gravitational field of a spherical mass.Model A.: Contraction through condensation of a polytropic respectively isothermal gas sphere.Model B: Condensation in the isothermal atmosphere which surrounds a core.Model B is sooner possible, because model A introduces certain restrictions of mass and radius of the protostar. 相似文献
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We consider a generalization of the Standard Model whose action displays conformal invariance in d dimensions. The model contains a strongly coupled dark matter sector which breaks conformal symmetry dynamically. The model evades conformal anomaly and leads to identically zero vacuum energy in flat space-time. Hence it does not suffer from the problem of fine tuning of the cosmological constant. We determine the contribution of non-relativistic matter to the energy-momentum tensor and determine a parameter regime in which it approximately reduces to the standard result. We show how dark energy and dark matter arises in this model. We discuss the parameter range for which the model reduces to the ΛCDM model and hence is consistent with observations. 相似文献