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1.
Our main goal is to determine the dynamic equations of a certain complex system, as is the case of the mechanical system for a small aperture telescope. Causes of this complexity are: the lack of documents about the operation of the elements belonging to the system, and the variation of dynamics with respect to the time and the position of the telescope. To check that we have obtained a valid set of dynamic equations, we will design a computer control system that will implement a self-guide system for the telescope. This revised version was published online in July 2006 with corrections to the Cover Date.  相似文献   

2.
一个巨型望远镜方案   总被引：4，自引：0，他引：4  
提出一个有特色的巨型望远镜(FGT)方案．其主镜口径为30米，主焦比为1．2，由1095块圆环形子镜构成．采用地平式装置．光学系统包括Nasmyth系统、折轴(Coude)系统和一个大视场系统．提出一个由4个镜面组成的新的Nasmyth系统，在约10′的视场范围内像斑小于爱里斑，达到衍射极限．比传统的Nasmyth系统的衍射极限视场大得多．可在这样的大视场内同时作好几个小区域的衍射极限的观测．当由Nasmyth系统转换到折轴系统和大视场系统时，采用主动光学技术改变子镜的面形、倾斜和平移，产生一个新的主镜面形，使折轴系统和大视场系统都能得到很好的像质．大视场系统的视场直径25′，场曲轻微，并有可能校正大气色散．给出了子镜面形和位置的公差，并讨论了望远镜的装置和结构,方案中的特色和创新对未来大望远镜的研制有普遍意义．  相似文献   

3.
We present families of symmetric and asymmetric periodic orbits at the 1/1 resonance, for a planetary system consisting of a star and two small bodies, in comparison to the star, moving in the same plane under their mutual gravitational attraction. The stable 1/1 resonant periodic orbits belong to a family which has a planetary branch, with the two planets moving in nearly Keplerian orbits with non zero eccentricities and a satellite branch, where the gravitational interaction between the two planets dominates the attraction from the star and the two planets form a close binary which revolves around the star. The stability regions around periodic orbits along the family are studied. Next, we study the dynamical evolution in time of a planetary system with two planets which is initially trapped in a stable 1/1 resonant periodic motion, when a drag force is included in the system. We prove that if we start with a 1/1 resonant planetary system with large eccentricities, the system migrates, due to the drag force, along the family of periodic orbits and is finally trapped in a satellite orbit. This, in principle, provides a mechanism for the generation of a satellite system: we start with a planetary system and the final stage is a system where the two small bodies form a close binary whose center of mass revolves around the star.  相似文献   

4.
The ultimate purpose of this investigation is the development of a world model or at least a skeleton for a world model, consisting of a finite number of material particles and of a finite number of geometrical points and time instants. The fundamental argument in the present article is the fact, that in the quantum theory we have to do with separable HILBERT spaces. The separable HILBERT spaces can be represented by means of linear operators with discrete eigenvalues and their eigenvectors. It is possible to replace the discrete eigenvalues with, for instance, non-negative integers, and these in their turn with numbers of a GALOIS field. In such a way a finitized physical system seems possible, or, if not a complete system, in any case a “skeleton” for a system. How far such a system might be developed remains an open question.  相似文献   

5.
A configuration for the Future Giant Telescope is proposed. It is a 30m telescope with segmented primary mirror and alt-azimuth mounting. The aspherical f/1.2 primary mirror is made up of 1095 partial annular submirrors. The optical system includes a Nasmyth system, a coude system and a wide field system. The Nasmyth system has a novel design with four mirrors and provides a ∼10 arcmin field of diffraction-limited images, a much larger field than can be obtained by the traditional Nasmyth system. Several diffraction-limited observations each over a small field, can be carried out simultaneously. By applying active optics to change the shape, tip, tilt and piston of the submirrors, thereby to effect a new aspherical surface of the primary, excellent quality images can be obtained for the coude system and the wide field system. The wide field system has a field of 25 arcmin, the focal surface is only slightly curved and the atmospheric dispersion could be corrected. The tolerances of the surface shape and position for the submirrors, and the telescope mounting and structure are also discussed. The innovations in this configuration should have a general significance for future giant telescopes.  相似文献   

6.
We study orbital evolution of multi-planet systems with masses in the terrestrial planet regime induced through tidal interaction with a protoplanetary disk assuming that this is the dominant mechanism for producing orbital migration and circularization. We develop a simple analytic model for a system that maintains consecutive pairs in resonance while undergoing orbital circularization and migration. This model enables migration times for each planet to be estimated once planet masses, circularization times and the migration time for the innermost planet are specified. We applied it to a system with the current architecture of Kepler 444 adopting a simple protoplanetary disk model and planet masses that yield migration times inversely proportional to the planet mass, as expected if they result from torques due to tidal interaction with the protoplanetary disk. Furthermore the evolution time for the system as a whole is comparable to current protoplanetary disk lifetimes. In addition we have performed a number of numerical simulations with input data obtained from this model. These indicate that although the analytic model is inexact, relatively small corrections to the estimated migration rates yield systems for which period ratios vary by a minimal extent. Because of relatively large deviations from exact resonance in the observed system of up to 2 %, the migration times obtained in this way indicate only weak convergent migration such that a system for which the planets did not interact would contract by only \({\sim }1\,\%\) although undergoing significant inward migration as a whole. We have also performed additional simulations to investigate conditions under which the system could undergo significant convergent migration before reaching its final state. These indicate that migration times have to be significantly shorter and resonances between planet pairs significantly closer during such an evolutionary phase. Relative migration rates would then have to decrease allowing period ratios to increase to become more distant from resonances as the system approached its final state in the inner regions of the protoplanetary disk.  相似文献   

7.
The reference system defined by Veis and currently used for computing satellite orbits is not sufficiently accurate for some scientific applications, considering the new accuracy of laser data. We have therefore defined another orbital reference system with associated apparent forces. The reference system chosen is the mean celestial system 1970.0. The motion of a satellite is numerically integrated in the instantaneous celestial system (sideral system), taking into account all the complementary forces due to precession and nutation. The complete set of formulas is given here and has been introduced in a differential orbital improvement program.  相似文献   

8.
We present a low cost meteor observation system based on the radio forward scattering and interferometry technique at Kochi University of Technology (KUT). The system can be a suitable model for low budget educational institutes that target practical learning of astronomical objects and upper atmospheric characteristics. The system methodology for the automatic counting of meteor echoes, filtering noise and detecting meteor echo directions is described. Detection of the meteor echo directions, which is the basic element for determining the meteor trajectories and the orbital parameters of parent comets, is based on a software system developed for analysis of phase differences detected by interferometry. Randomly selected observation samples measured by the radio interferometer are compared to simultaneous optical observations by video cameras to verify the system accuracy. Preliminary error analysis revealed that the system accuracy is directly related to the duration of observed meteor echoes. Eighty percent of meteor echo samples with durations longer than 3 s showed agreement in azimuth and elevation angles measurements to within a 10° error range, while meteor echo samples with shorter durations showed lower agreement levels probably due to the low system sampling resolution of 0.1 s. The reasonable agreement level of meteor echoes with duration longer than 3 s demonstrated the applicability of the system methodology. Accurate observation of shorter duration meteor echoes could possibly be achieved by improving the system resolution.  相似文献   

9.
A computer experiment on a one-dimensional self-gravitating system is described. We attempt to observe the dynamic time required for this system to thermalize by comparing the position and velocity densities with those predicted by the microcanonical ensemble. Hohl and Broaddus (1967) have previously reported an estimate of the thermalization time which is inferred from studies of the kinetic energy covariance. We ran the system for the time which they report and find that the system has not thermalized. Furthermore, there is no evidence that the system is even proceeding towards equilibrium in the time-scale considered here. Significant changes in the distribution do occur in a short time, after which the system remains in a stationary state which is not characteristic of equilibrium.  相似文献   

10.
We examine the possibility that ε Carinae is a triple system. We show that a stable hierarchical system is possible, although perhaps only marginally.
We outline a speculative scenario for the history of the system, in which the giant outburst of the last century is associated with an interchange of components in a dynamically unstable triple system. We point out that the currently observed spectroscopic 'event' could be used to distinguish among the different possible configurations of the system.  相似文献   

11.
本文指出了子午环光栏自动控制系统研制的必要性，并简要介绍了控制原理．结果表明，该控制部分设计合理大大简便了操作．  相似文献   

12.
There are four systems of a massive central body with a regularily structured satellite system in the Solar system: the planetary system and the satellite systems of Jupiter, Saturn and Uranus. Comparable structures in these four systems can be understood as indications for comparable processes of origin and formation. It is the aim of this paper to describe comparable properties, and to discuss possible physical processes in pre-satellite disks which can be the cause for this comparability.  相似文献   

13.
The objective of this project is to develop and construct an innovative imaging system for nuclear medicine and molecular imaging that uses photon diffraction and is capable of generating 1–2 mm spatial resolution images in two or three dimensions. The proposed imaging system would be capable of detecting radiopharmaceuticals that emit 100–200 keV gamma rays which are typically used in diagnostic nuclear medicine and in molecular imaging. The system is expected to be optimized for the 140.6 keV gamma ray from a Tc-99m source, which is frequently used in nuclear medicine. This new system will focus the incoming gamma rays in a manner analogous to a magnifying glass focusing sunlight into a small focal point on a detector's sensitive area. Focusing gamma rays through photon diffraction has already been demonstrated with the construction of a diffraction lens telescope for astrophysics and a scaled-down lens for medical imaging, both developed at Argonne National Laboratory (ANL). In addition, spatial resolutions of 3 mm have been achieved with a prototype medical lens. The proposed imaging system would be comprised of an array of photon diffraction lenses tuned to diffract a specific gamma ray energy (within 100–200 keV) emitted by a common source. The properties of photon diffraction make it possible to diffract only one specific gamma ray energy at a time, which significantly reduces scattering background. The system should be sufficiently sensitive to the detection of small concentrations of radioactivity that can reveal potential tumor sites at their initial stages of development. Moreover, the system's sensitivity would eliminate the need for re-injecting a patient with more radiopharmaceutical if this patient underwent a prior nuclear imaging scan. Detection of a tumor site at its inception could allow for an earlier initiation of treatment and wider treatment options, which can potentially improve the chances for cure.  相似文献   

14.
A new integration theory is formulated for dynamical systems with two degrees of freedom, in the gravitational field of a rotating system. Four integrals of motion may be determined from complete solutions of a system of three first-order, partial differential equations in three independent variables. The solutions of this system define two integral surfaces with space-time coordinates. These surfaces represent two independent solutions of a second-order kinematic system to which the original fourth-order system has been reduced. An integral curve may be represented as the locus of intersection points of the integral surfaces. The new theory is the theoretical basis for a method of analytic continuation of periodic orbits of the circular restricted problem.  相似文献   

15.
Stability of Binary Asteroids   总被引：1，自引：0，他引：1  
D.J. Scheeres 《Icarus》2002,159(2):271-283
The stability and final outcome of a strongly interacting binary asteroid system is considered. We discuss the implications of the system transferring energy and angular momentum between rotational and translational motion while conserving the total system energy and angular momentum. Using these results we can develop a set of sufficient conditions for stability against escape and impact. These allow us to delineate several classes of final outcomes for a binary asteroid system, each of which may have implications for asteroid observations. The effects of energy dissipation on an asteroid binary system are also considered and are shown to be able to change the stability of the system against escape and impact. An example computation for the near-Earth asteroid binary 1996 FG3 is given along with a series of numerical explorations of an evolving binary system consisting of an ellipsoid and a sphere of equal mass.  相似文献   

16.
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。  相似文献   

17.
Photoelectric observations in B and V for the FZ Del system are presented and its light curves are analyzed. Absolute parameters are obtained. The system shows a near contact subgaint secondary component with a likely K1 spectral type. The O-C curve is presented and probably a secular orbital period variations is detected on a timescale of about 6.9×106 yrs, suggesting thermal timescale mass transfer. A new light elements for the system have been obtained. The system can be considered as an early stage of conservative case of mass transfer. This revised version was published online in August 2006 with corrections to the Cover Date.  相似文献   

18.
When gravitational aggregates are spun to fission they can undergo complex dynamical evolution, including escape and reconfiguration. Previous work has shown that a simple analysis of the full 2-body problem provides physically relevant insights for whether a fissioned system can lead to escape of the components and the creation of asteroid pairs. In this paper we extend the analysis to the full 3-body problem, utilizing recent advances in the understanding of fission mechanics of these systems. Specifically, we find that the full 3-body problem can eject a body with as much as 0.31 of the total system mass, significantly larger than the 0.17 mass limit previously calculated for the full 2-body problem. This paper derives rigorous limits on a fissioned 3-body system with regards to whether fissioned system components can physically escape from each other and what other stable relative equilibria they could settle in. We explore this question with a narrow focus on the Spherical Full Three Body Problem studied in detail earlier.  相似文献   

19.
We have been carrying out solar wind measurements using the interplanetary scintillation (IPS) method. Our IPS observation system is operated at a frequency of 327MHz and consists of four stations located at Toyokawa, Fuji, Sugadaira and Kiso. The present system, however, has insufficient sensitivity to measure enough IPS sources for observing the solar wind with adequate spatial and temporal resolution. Therefore we have been excuting the upgrade project since 1994 in order to observe a larger number of compact radio sources. The Fuji system has been improved successfully and has achieved sensitivity by a factor over five compared with the previous system. The upgrade project is now in progress for the Toyokawa and Sugadaira station.  相似文献   

20.
Frequency analysis is a new method for analyzing the stability of orbits in a conservative dynamical system. It was first devised in order to study the stability of the solar system (Laskar, Icarus, 88, 1990). It is a powerful method for analyzing weakly chaotic motion in hamiltonian systems or symplectic maps. For regular motions, it yields an analytical representation of the solutions. In cases of 2 degrees of freedom system with monotonous torsion, precise numerical criterions for the destruction of KAM tori can be found. For a 4D symplectic map, plotting the frequency map in the frequency plane provides a clear representation of the global dynamics and describes the actual Arnold web of the system.  相似文献   

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