圆轨道锥束重建精度与锥角关系的研究   总被引：5，自引：1，他引：5  

曾凯  陈志强  张丽  赵自然 《CT理论与应用研究》2003,12(3):9-16

目的：深入研究Radon空间的数据缺失与锥角的关系改进算法。方法：相对于二维CT重建，锥束重建有着诸多优势，因此目前得到越来越广泛的应用。圆轨道锥束重建，因为算法上的简洁性以及工程实现的可行性，成为了锥束重建比较乐于采用的形式。但是由于圆轨道几何结构的限制，使其不能够得到完备的锥束重建数据，只有在锥角较小的情况下才能得到，因此深入研究Radon空间的数据缺失与锥角的关系以改进算法。结果：通过一定的近似得到了一个它们之间比较简单的关系。结论：基于这一关系提出了改进算法  相似文献   

Tidal torques: a critical review of some techniques     

Michael Efroimsky  James G. Williams 《Celestial Mechanics and Dynamical Astronomy》2009,104(3):257-289

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A Research on the Orbit Determination Method by Means of Sparse Data of Electronic Fences     

Cao Zhi-bin  Xu Jin  Ma Jian-bo  Hu Wei-dong  Fang Ai-li 《Chinese Astronomy and Astrophysics》2009

Based on the Lambert equation and knowledge of space geometry a method of orbit determination is given using the sparse observational data provided by the space monitoring electronic fence device. Our simulated experiment of a large number of targets shows that the initial orbit determined by this method can be improved and can converge to a final accuracy better than 100 m, so proving that the method can be applied to the orbit determination of an overwhelming majority of space targets with the observed data of the electronic fence. Finally, the effect of the latitude of the observing station on the application of the method is discussed.  相似文献   

On the oscillations in Mercury's obliquity     

E. Bois  N. Rambaux   《Icarus》2007,192(2):308-317

Mercury's capture into the 3:2 spin–orbit resonance can be explained as a result of its chaotic orbital dynamics. One major objective of MESSENGER and BepiColombo spatial missions is to accurately measure Mercury's rotation and its obliquity in order to obtain constraints on internal structure of the planet. Analytical approaches at the first-order level using the Cassini state assumptions give the obliquity constant or quasi-constant. Which is the obliquity's dynamical behavior deriving from a complete spin–orbit motion of Mercury simultaneously integrated with planetary interactions? We have used our SONYR model (acronym of Spin–Orbit N-bodY Relativistic model) integrating the spin–orbit N-body problem applied to the Solar System (Sun and planets). For lack of current accurate observations or ephemerides of Mercury's rotation, and therefore for lack of valid initial conditions for a numerical integration, we have built an original method for finding the libration center of the spin–orbit system and, as a consequence, for avoiding arbitrary amplitudes in librations of the spin–orbit motion as well as in Mercury's obliquity. The method has been carried out in two cases: (1) the spin–orbit motion of Mercury in the 2-body problem case (Sun–Mercury) where an uniform precession of the Keplerian orbital plane is kinematically added at a fixed inclination (S_2K case), (2) the spin–orbit motion of Mercury in the N-body problem case (Sun and planets) (S_n case). We find that the remaining amplitude of the oscillations in the S_n case is one order of magnitude larger than in the S_2K case, namely 4 versus 0.4 arcseconds (peak-to-peak). The mean obliquity is also larger, namely 1.98 versus 1.80 arcminutes, for a difference of 10.8 arcseconds. These theoretical results are in a good agreement with recent radar observations but it is not excluded that it should be possible to push farther the convergence process by drawing nearer still more precisely to the libration center. We note that the dynamically driven spin precession, which occurs when the planetary interactions are included, is more complex than the purely kinematic case. Nevertheless, in such a N-body problem, we find that the 3:2 spin–orbit resonance is really combined to a synchronism where the spin and orbit poles on average precess at the same rate while the orbit inclination and the spin axis orientation on average decrease at the same rate. As a consequence and whether it would turn out that there exists an irreducible minimum of the oscillation amplitude, quasi-periodic oscillations found in Mercury's obliquity should be to geometrically understood as librations related to these synchronisms that both follow a Cassini state. Whatever the open question on the minimal amplitude in the obliquity's oscillations and in spite of the planetary interactions indirectly acting by the solar torque on Mercury's rotation, Mercury remains therefore in a stable equilibrium state that proceeds from a 2-body Cassini state.  相似文献   

Space VLBI Geodesy: background of an experiment proposal     

I. Fejes  N. Kawaguchi  Sz. Mihály 《Astrophysics and Space Science》1996,239(2):275-280

Space VLBI is a new observing technique which will be available in the second half of this decade by radio telescopes as interferometer elements in orbit. Besides the main astronomical interests, this new development has some very interesting potential applications in satellite dynamics, geodesy and geodynamical research which qualify space VLBI a potential new technique in space geodesy. A geodesy demostration experiment (GEDEX) is being proposed for the Japanese space VLBI satellite-VSOP, with the main objectives of reference frame interconnections and orbit accuracy improvement of the space radio telescope. The paper gives a review of the special characteristics of space VLBI and a general background of the GEDEX proposal.  相似文献   

P/GE-Wang joins P/Slaughter-Burnham and P/Boethin in the club of comets in 1/1 resonance with jupiter     

Daniel G. Benest 《Celestial Mechanics and Dynamical Astronomy》1989,47(4):361-374

Three comets are now known to be at or near the 1/1 resonance with Jupiter P/Slaughter-Burnham, P/Boethin and the newly discovered P/Ge-Wang. Their orbital evolutions are compared, using the elliptic three-dimensional restricted three-body model Sun-Jupiter-comet. Although details of the individual orbits differ, the three comets have very similar general dynamical behaviours, and stay during a long time at or near the 1/1 resonance, at least for several thousand years.  相似文献   

极轨道卫星上测量太阳常数的新方法   总被引：4，自引：0，他引：4  

方伟  禹秉熙 《遥感学报》1997,1(4):241-245

该文提出了一种在极轨道太阳同步卫星上，利用指向太阳矢量方向安装的绝对辐射汁，以非跟踪方式测量太阳常数的方法，非跟踪模式下简化模型热力学微分方程解与跟踪模式的解形式相似，微机模拟画出二模式下的能量响应曲线，二曲线在最高点基本重合，表明这种方法同样能够达到太阳进行测量的精度，且结构简单，测量方便。  相似文献   

星载海洋高度计应用对测轨精度的要求     

马树斌 《海洋科学进展》1994,(4)

本文通过动力海洋学的典型空间尺度与ＯＥＯ－３，ＳＥＡＳＡＴ，ＧＥＯＳＡＴ和ＴＯＰＥＸ／Ｐｏｓｅｉｄｏｎ等卫星高度计测量高度的精度作比较，将星戴高度计应用对测轨精度的要求作了总结．对大多数海洋学研究来说、应用卫星高度计数据要求测轨精度达到数十厘米  相似文献   

Video observations, atmospheric path, orbit and fragmentation record of the fall of the Peekskill meteorite     

Z. Ceplecka  P. Brown  R. L. Hawkes  G. Wetherill  M. Beech  K. Mossman 《Earth, Moon, and Planets》1995,71(3):395-404

Large Near-Earth-Asteroids have played a role in modifying the character of the surface geology of the Earth over long time scales through impacts. Recent modeling of the disruption of large meteoroids during atmospheric flight has emphasized the dramatic effects that smaller objects may also have on the Earth's surface. However, comparison of these models with observations has not been possible until now. Peekskill is only the fourth meteorite to have been recovered for which detailed and precise data exist on the meteoroid atmospheric trajectory and orbit. Consequently, there are few constraints on the position of meteorites in the solar system before impact on Earth. In this paper, the preliminary analysis based on 4 from all 15 video recordings of the fireball of October 9, 1992 which resulted in the fall of a 12.4 kg ordinary chondrite (H6 monomict breccia) in Peekskill, New York, will be given. Preliminary computations revealed that the Peekskill fireball was an Earth-grazing event, the third such case with precise data available. The body with an initial mass of the order of 10⁴ kg was in a pre-collision orbit with a = 1.5 AU, an aphelion of slightly over 2 AU and an inclination of 5. The no-atmosphere geocentric trajectory would have lead to a perigee of 22 km above the Earth's surface, but the body never reached this point due to tremendous fragmentation and other forms of ablation. The dark flight of the recovered meteorite started from a height of 30 km, when the velocity dropped below 3 km/s, and the body continued 50 km more without ablation, until it hit a parked car in Peekskill, New York with a velocity of about 80 m/s. Our observations are the first video records of a bright fireball and the first motion pictures of a fireball with an associated meteorite fall.  相似文献   

Unified iterative methods in orbit determination     

C. Dumoulin 《Celestial Mechanics and Dynamical Astronomy》1994,59(1):73-89

The classical problem of Keplerian orbit determination from only three measurements of time and angular coordinates (t _i, _i, _i) has been solved here numerically in two different ways, using Newton's method for non-linear equations in both cases. The first method (Perov, 1989) is based on KS variables, whereas the second emphasizes the fundamental part played by the unified Lambert's equation and the related formulae in that kind of applications. These two methods have been compared and put into practice in various numerical tests based on real asteroid orbits and ficitious Keplerian asteroid, comet and artificial satellite orbits in order to try the stability of these methods for peculiar orbits.  相似文献