共查询到18条相似文献，搜索用时 109 毫秒
1.
针对长焦距望远镜CCD观测天然卫星的情况，导出了用两颗亮星作为定标时，CCD视场几何参数(比例尺和指向)测量的误差公式，进而设计了多定标星定标时正确的归算方案。新方案不仅对天然卫星的位置测量，也对同类型的小视场CCD位置测量具有指导意义。 相似文献
2.
针对长焦距望远镜CCD观测天然卫星的情况,导出了用两颗亮星作为定标时,CCD视场几何参数(比例尺和指向)测量的误差公式,进而设计了多定标星定标时正确的归算方案。新方案不仅对天然卫星的位置测量,也对同类型的小视场CCD位置测量具有指导意义。 相似文献
3.
1995年天王星卫星位置观测的重新归算 总被引：4，自引：3，他引：1
研究改进了对自然卫星CCD图像进行定位量测处理的方法。经对天王星主要卫星CCD观测位置图像的计算处理表明位置精度有了明显提高 ,O -C的标准误差 (RMS)平均为 0 .0 7″。 相似文献
4.
暗弱天然卫星与主带小行星相比,具有亮度低、速度变化快的特点.在观测这类天体时,不能简单地延长曝光时间来提高其信噪比.尝试观测多幅短曝光的CCD (chargecoupled device)图像,采用移位堆叠(shift-and-add)方法,希望提高目标成像的信噪比,获得暗弱天然卫星的精确测量结果.使用2018年4月9—12日夜间,中国科学院云南天文台1 m望远镜(1 m望远镜)拍摄的木星5颗暗卫星的229幅CCD图像,实施了移位堆叠试验.为了验证结果的正确性,与相近日期中国科学院云南天文台2.4 m望远镜(2.4 m望远镜)观测的相同木卫图像的测量结果进行了比较和分析.位置归算采用了JPL (Jet Propulsion Laboratory)历表.结果表明,对CCD图像使用移位堆叠方法,通过叠加约10幅曝光时间100 s的图像, 1 m望远镜能观测暗至19等星的不规则天然卫星,而且测量的准确度与2.4 m望远镜的测量结果有良好的一致性. 相似文献
5.
用M15进行CCD视场的校准 总被引：3，自引：2，他引：1
用1996年10月所获得的球状星团M15和大距离双星61Cygni的CCD观测资料,分别求解了上海天文台1.56m天体测量望远镜上安装的CCD探测器视场的位置角改正δp和尺度因子ρ。通过对土星主要卫星观测资料0－C的计算分析表明,经球状星团校准视场后所得结果较双星校准后结果的精度要高。该结论为进一步提高计算大行星卫星的位置测量精度打下良好的基础。 相似文献
6.
CCD在空间天体测量上的应用 总被引：1，自引：0，他引：1
本文分析了依巴谷空间天体测量卫星主探测器析像管和恒星测绘仪的工作缺点;介绍了用CCD作为HIPPARCOS主探测器的优越性,预期的观测结果,以及误差分析比较。 相似文献
7.
本论述了利用GPS卫星的射电与光学定位实现参考系连接的基本方法,并对参考系连接的精度作了分析，探讨了中国VLBI网利用GPS卫星进行参考系连接的可能性。章认为以VLBI、CCD技术为观测手段，利用GPS卫星可使射电参考系与恒星参考系在0.″01甚至更高的精度上得到连接。 相似文献
8.
《天文研究与技术》2017,(3)
在地面望远镜观测土星主要卫星的精确定位中,目前普遍采用CCD成像技术。为了测量视场中暗卫星的位置,常采用4颗主要卫星(土卫三-土卫六)进行定标。鉴于技术的进步,目前CCD视场正在逐步增加,如何精确定标图像值得研究。利用2010年1月20日在云南天文台1 m望远镜上观测的不同取向的105幅CCD图像进行了试验研究。采用了美国喷气推进实验室土星主要卫星历表和美国海军天文台的UCAC4恒星星表进行计算,相对于不同的参考对象进行定标。结果表明,采用4颗主要卫星进行定标并测量离卫星较近的观测对象时具有较好的测量准确度和内部精度。测量离定标星较远的卫星时,这种定标方法具有较大的不确定性。采用6颗主要卫星(土卫三-土卫八)进行定标,所有卫星的测量结果具有更好的外部和内部符合。即便如此,采用四常数模型和六常数模型定标的结果都不是令人满意,这揭示CCD视场存在明显的扭曲效应。如果采用视场中的恒星定标,卫星的外部符合和内部精度明显变差,这说明UCAC4恒星参考星表也不是理想的定标用参考星表。 相似文献
9.
为了满足大行星卫星的高精度CCD位置观测与运动理论研究工作的需要 ,采用天王星 5颗主要卫星摄动理论模型 (Gust86 )作为核心 ,设计了一个天王星视位置可视化软件。该软件具有卫星证认 ,最佳观测时段选取 ,精确模拟卫星视运动和实时引导CCD精密定位观测等功能。 相似文献
10.
近20年来，随着CCD和像增强器的发展，小巧灵活的流星视频观测系统在世界上逐渐多了起来．并且，最终将可能逐步取代流星的目视观测和普通照相观测．介绍云南天文台I号流星彗星视频照相系统的研制及其初步观测结果．这一系统由容易转换的5组件构成．用于流星观测的大视场相机的视场约36度，单帧图像可观测到约6等恒星．实测的恒星星等测量精度可达约0.2等．还讨论了视频照相机比传统的感光胶卷照相的长处，以及视频照相系统的改进与发展． 相似文献
11.
Abstracts—A special method of ground-based observations of natural planetary satellites is described. A higher accuracy of observations is reached at the periods of their visible encounters as two satellites fall within the same CCD frame. For the outermost natural satellites, such events are very rare. The circumstances of the visible encounters of the outermost satellites of Jupiter are precalculated for two years to come and are presented in this paper. The observations of these satellites are particularly important in solving the problems connected with the origin and evolution of small bodies in the Solar System. 相似文献
12.
天然卫星的位置测量在天体测量和天体力学中都有重要意义。国外有人对天王星卫星位置测量应用新的图象处理方法得到了高精度的卫星观测资料。利用云南天文台１米望远镜上获得的两颗卫星的ＳＲＴ的ＣＣＤ观测资料进行了新老图象处理方法的比较研究。当用两颗卫星直接作定标测量ＣＣＤ的比例尺和指向时表明：主星晕的处理对卫星位置的测量非常重要。去晕处理后,测得的比例尺和指向的弥散将大为减少。 相似文献
13.
T. P. Kiseleva A. A. Kiselev O. A. Kalinichenko N. A. Vasilyeva M. L. Khovricheva 《Solar System Research》2008,42(5):414-433
The results of photographic observations of Jupiter’s Galilean satellites made with the 26-inch refractor at the Pulkovo Observatory from 1986 to 2005 are given. Satellite coordinates with respect to Jupiter and the mutual distances between the satellites have been determined. A scale-trale technique that does not require reference stars for the astrometric reduction of measurements has been used. The effect of the Jupiter phase has been taken into account in the jovicentric coordinates. The observation results have been compared with a modern theory of the Galilean satellites’ motions. Systematic observation errors depending on the observation technique have been studied. The intrinsic observation accuracy in the random quotient is characterized by the values 0.041″ over X and Y. The external accuracy of the relative Galilean satellite coordinates determined by comparing the observations with modern ephemerides turned out to be equal to 0.165″, 0.213″ for the Jovicentric coordinates and 0.134″, 0.170″ for the “satellite-satellite” coordinates. The highest accuracy of the relative satellite coordinates is reached at small distances between the satellites which are less than 100″: the corresponding mean-square errors of one observation are equal in to the external convergence to 0.050″, 0.070″. The results of photographic observations have been compared with the first CCD observations of the Jupiter satellites made in 2004 with the 26-inch refractor. 相似文献
14.
A. L. Poroshina 《Astronomy Letters》2013,39(12):876-881
The ephemerides of satellites of major planets are needed in planning spacecraft missions both for studying the satellites themselves and for navigational support during the flights of spacecraft in the vicinity of planets. In addition, accurate numerical theories of motion of the natural satellites of major planets make it possible to increase the accuracy of the ephemerides of their central planets based on positional (photographic and CCD) observations of the satellites. Numerical theories of Neptune’s satellites, Triton and Nereid, constructed within the framework of the ERA software package developed at the Institute of Applied Astronomy of the Russian Academy of Sciences are presented. 相似文献
15.
天王星卫星的CCD观测与分析解的比对 总被引：2，自引：0，他引：2
本文给出了处理天王星卫星ＣＣＤ图象位置资料的新方法,并将我们在１９９５年取得的重要资料与两种理论模型位置进行了比较计算,结果表明经处理后的天王星五颗主要卫星ＣＣＤ观测精度有了较大提高。 相似文献
16.
T. P. Kiseleva I. S. Izmailov O. A. Kalinichenko T. A. Vasilieva 《Solar System Research》2010,44(1):60-67
The results of the reduction, investigation, and comparison of the photographic observations of the major Saturnian satellites
and CCD observations with an ST6 CCD camera obtained at the 264nch Pulkovo refractor in 1995–2007 are presented. A comparison
of the observational results with the TASS 1.7 theory of motion of the Saturnian satellites has served as the basis for investigating
and comparing the series of observations. The period-averaged (O-C) residuals and observational errors have been calculated.
A comparison of the series of CCD and photographic observations has shown the same external accuracy of the observations at
a higher internal accuracy of the CCD observations than that of the photographic ones. A comparison of the Pulkovo results
with those of other authors has shown them to be close in accuracy. The accuracy of the theory has been estimated by comparing
simultaneous (on the same night) CCD and photographic observations. The errors of the observations and the theory have been
found from this comparison to be the following: 0.081“ and 0.067” for the observations and 0.077“ and 0.115” for the theory
(inxandy, respectively). An analysis of the dependence of (O-C)x,y for three satellites (the sixth, seventh, and eighth) on the satellite positions in Saturn-centered orbits has revealed systemat
ic deviations for the seventh satellite in both coordinates. The positions of Saturn have been determined from satellite observations
without measuring its images on photographic plates with accuracies of 0.121“ and 0.105” in right ascension and declination,
respectively. 相似文献
17.
利用新发表的高精度、高密度天体测量星表UCAC2,对天王星的五颗主要卫星的CCD观测图像重新进行量测,采用不同方法作定标归算,并使用两种理论模型(GUST86和GUST06模型)计算卫星的理论位置。对不同方法所得到的卫星位置的O-C结果的分析和比较表明,本文获得的卫星位置精度,除天卫五(Miranda)有显著提高,其他4颗卫星的位置精度基本相同。本文中天卫一和天卫三的结果与"亮卫星定标法"的结果在精度上相当,天卫二的位置精度与其他天王星卫星的位置精度具有较好的一致性,这从另一方面证明了我们的"亮卫星定标法"的可靠性。此外我们还获得了天卫四的位置与精度。 相似文献
18.
After a CCD image of the four Galilean satellites of Jupiter is obtained by a long focal length telescope, we can compare the theoretical positions of these satellites with their pixel positions so as to obtain the calibration parameters of the CCD field of view. In theory, when two of the four satellites have small enough separation, their relative positional measurement will have a good accuracy since the error existing in the solved calibration parameters has a direct proportional effect on the separation of the two satellites. The 347 CCD images taken by 1-m long focal length telescope at Yunnan Observatory in 2002-2005 are used to perform the experimental test. After we improve the centroid algorithm for the satellites and our former halo-removal technique, the results show that the positional measurement of two small-separation satellites has an external precision as good as 0.01-0.03 arcsec. This precision has comparability as that from rarely occurring mutual events of the Galilean satellites. This experiment confirms the finding of the “precision premium” firstly presented by Pascu [1994. An appraisal of the USNO program of photographic astrometry of bright planetary satellites. In: Morrison, L.V., Gilmore, G.F., (Eds.), Galatic and Solar System Optical Astrometry, pp. 304-311] using photographic observations. We believe that this type of observations, besides mutual event observations, might also be used to improve our knowledge of the orbital motions of the Galilean satellites because of its much more opportunities. 相似文献