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Astrometry of the main satellites of Uranus: 18 years of observations

机译:天王星主要卫星的占星术:18年的观测

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Context. We contribute to developing dynamical models of the motions of Uranus’ main satellites. Aims. We determine accurate positions of the main satellites of Uranus: Miranda, Ariel, Umbriel, Titania, and Oberon. Positions of Uranus, as derived from those of these satellites, are also determined. The observational period spans from 1992 to 2011. All runs were made at the Pico dos Dias Observatory, Brazil. Methods. We used the software called Platform for Reduction of Astronomical Images Automatically (PRAIA) to perform a digital coronography to minimise the influence of the scattered light of Uranus on the astrometric measurements and to determine accurate positions of the main satellites. The positions of Uranus were then indirectly determined by computing the mean differences between the observed and ephemeris positions of these satellites. A series of numerical filters was applied to filter out spurious data. These filters are mostly based on (a) the comparison between the positions of Oberon with those of the other satellites and on (b) the offsets as given by the differences between the observed and ephemeris positions of all satellites. Results. We have, for the overall offsets of the five satellites, ?29 mas (±63 mas) in right ascension and ?27 mas (±46 mas) in declination. For the overall difference between the offsets of Oberon and those of the other satellites, we have +3 mas (±30 mas) in right ascension and ?2 mas (±28 mas) in declination. Ephemeris positions for the satellites were determined from DE432+ura111. Comparisons using other modern ephemerides for the solar system – INPOP13c – and for the motion of the satellites – NOE-7-2013 – were also made. They confirm that the largest contribution to the offsets we find comes from the motion of the barycenter of the Uranus system around the barycenter of the solar system, as given by the planetary ephemerides. For the period from 1992 to 2011, our final catalogues contain 584 observed positions of Miranda, 1710 of Ariel, 1987 of Umbriel, 2588 of Titania, 2928 of Oberon, and 3516 of Uranus.
机译:上下文。我们致力于开发天王星主要卫星运动的动力学模型。目的我们确定天王星主要卫星的准确位置:米兰达,爱丽儿,雨伞,二氧化钛和奥伯龙。还确定了从这些卫星的位置得出的天王星的位置。观测期从1992年到2011年。所有运行均在巴西的皮科多斯迪亚斯天文台进行。方法。我们使用名为“自动减少天文图像的平台”(PRAIA)的软件进行数字冠状图检查,以最大程度地减少天王星散射光对天体测量的影响,并确定主要卫星的准确位置。然后通过计算这些卫星的观测星历和星历位置之间的平均差间接确定天王星的位置。应用了一系列数值滤波器来滤除虚假数据。这些滤波器主要基于(a)Oberon位置与其他卫星的位置之间的比较,以及(b)所有卫星的观测星历和星历位置之间的差异所给出的偏移。结果。对于这五颗卫星的总偏移量,右上角为?29 mas(±63 mas),偏角为?27 mas(±46 mas)。对于Oberon和其他卫星的偏移之间的总体差异,我们在右上角的偏移量为+3 mas(±30 mas),在赤纬方向上的偏移量为?2 mas(±28 mas)。卫星的星历位置由DE432 + ura111确定。还对使用其他现代星历表进行的太阳系INPOP13c和卫星运动NOE-7-2013进行了比较。他们证实,对我们发现的偏移量的最大贡献来自行星星历表给出的天王星系统重心围绕太阳系重心的运动。从1992年到2011年,我们的最终目录包含584个观察到的米兰达位置,1710个Ariel,1987年的Umbriel,2588个的Titania,2928个的Oberon和3516的天王星。

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