共查询到20条相似文献，搜索用时 78 毫秒
1.
基于哈特曼检测所求出的点列图分布，给出适用于天文望远镜的光学传递函数的测量方法；并给出云南天文台１．２ｍ地平式望远镜的光学传递函数值。 相似文献
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本文以声速点的物理量作为边界条件,积分流体力学方程组,给出了几何薄光学厚的黑洞吸积盘的温度分布.结果表明在这种吸积盘的内缘温度将急剧下降.另外,我们发现几何薄光学薄气体压为主的α-律吸积盘是热不稳定的. 相似文献
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利用北京天文台具有ＣＣＤ终端的６０ｃｍ光学望远镜（Ｖ波段）观测射电源的光学对应体，得到了０７１６＋７１４和０８３９＋１８７精确的光学位置。参考星表采用拉帕尔玛（ＬａＰａｌｍａ）的１８ｃｍ全自动子午环观测资料编制的ＣＡＭＣ星表，该星表是ＦＫ５星表系统。两颗源位置的内符精度约为０．″１９，与其他作者给出的光学和射电位置观测结果分别进行了比较 相似文献
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本文给出了１９９４年７月１７日至２２日，彗星碰撞期间，福州和乌鲁木齐两个观测点所取得的部分光学观测资料。 相似文献
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本文给出了１９９４年７月１７日至２２日，彗星碰撞期间，福州和乌鲁木齐两个观测点所取得的部分光学观测材料。 相似文献
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本文利用红外天文卫星点源表及哈勃望远镜导星星表对１９９０年新发表的７５个Ｓ星进行了ＩＲＡＳ红外源及ＧＳＣ光学对应体的证认，给出４１个Ｓ星有ＩＲＡＳ对应体，１２个Ｓ星有ＧＳＣ光学对应体。 相似文献
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１９９５年５月，使用２．１６ｍ望远镜对ＲＯＳＡＴ Ｘ射线源进行光学证认期间，发现８个ＲＯＳＡＴ Ｘ射线源和５Ｇ射电源的光学对应体是以前未发现的类星体，其红移范围从０．３３３至１．０９１。本文给出了这些类星体的多波段特性。 相似文献
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介绍与LAMOST低色散多目标光纤光谱仪五种方案对应的CCD照相机,每个照相机都给出了结构示意图和像斑直径的RMS值,并从多方面分析了它们各自的优缺点,章末节给出了低色散光谱仪最后的光学设计方案。 相似文献
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大气气溶胶和可降水量会影响天文望远镜光学成像系统的观测质量.利用中国科学院安徽光学精密机械研究所自主研制的DTF-6型太阳光度计观测了丽江高美古2010年10月～2011年5月的太阳直接辐射,获得了丽江高美古晴朗无云天气条件下气溶胶光学厚度(大气透明度)、(A)ngstr(o)m指数和可降水量;给出了该地区观测期间气溶胶光学厚度、(A)ngstr(o)m指数和大气可降水量的日变化与季节变化特征.实验期间,气溶胶光学厚度和可降水量日变化大致可分为4种类型,季节变化都呈现为冬季最小,秋季次之,春季升高.总体来说丽江高关古气溶胶光学厚度和可降水量都较小,该地区大气较清洁透明,且大气中积聚的多为小粒子,适用于天文观测. 相似文献
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德令哈13.7 m望远镜是中国最重要的射电望远镜之一.望远镜自安装超导成像频谱仪以及采用飞行观测模式以来,运行近10 yr.在此期间,望远镜开展并完成大量的天文观测,累积了巨量的天文数据,取得了一系列重要的科研成果.介绍了超导成像频谱仪在天文观测中的运行状态,运行中疑难问题、故障现象及解决方案.详述了超导成像频谱仪各方面性能测试及多年来的性能分析,包含接收机噪声温度及望远镜系统噪声温度、镜像抑制比、接收机稳定性、波束性能等方面.列举了超导成像频谱仪更新发展方面的工作,包含本振功率自动化调整、边带分离型超导混频器预放大电路的更新、控制程序的优化等.总结经验和规律,承前启后,将过去的超导成像频谱仪的维护运行经验应用到之后新一代大规模接收机系统中. 相似文献
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《Chinese Astronomy and Astrophysics》2021,45(4):559-586
Delingha 13.7 m telescope is one of the most important radio telescopes in China. Since installing the superconducting spectroscopic array receiver (SSAR) and adopting the On The Fly (OTF) observation mode, the telescope has operated for nearly 10 years. During this period, a large number of astronomical observation projects have been carried out and completed, a large amount of astronomical data have been accumulated, and a series of important scientific results have been achieved. This paper introduces the operating status of SSAR in astronomical observations, the problems in operations, as well as the fault phenomena and solutions. The performance test and performance analysis of SSAR are described in detail, including the receiver noise temperature and telescope system noise temperature, image rejection ratio (IRR), receiver stability, beam performance and so on. The updating and development of SSAR are listed, including the automatic adjustment of LO (Local Oscillator) power, the updating of pre-amplification circuits of the sideband separation superconducting mixer, and the optimization of control program, etc. This paper summarizes the experiences and rules, and connects the past with the future, for applying the experiences of the maintenance and operation of SSAR to the next-generation large-scale receiver system. 相似文献
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Dejonghe 《Monthly notices of the Royal Astronomical Society》1998,299(4):985-997
The general form of the surface density of an infinitely thin disc is given that generates a Sta¨ckel potential in the disc only, using formulae for the potential of elliptic and hyperbolic strings. This is useful for problems in which a simple form for the potential is important, while the corresponding surface density need only be known to check (numerically) that it is positive. A simple potential with a positive surface density is given. Also, formulae are given to calculate the surface density of such a Sta¨ckel disc, in the case in which the rotation curve is given and all the mass is concentrated in the disc. 相似文献
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Vladimír Matas 《Celestial Mechanics and Dynamical Astronomy》1978,17(2):193-194
The following is proved in this note: If we construct a circle passing through a given primary in the planar circular restricted three-body problem, center of which is the remaining primary, then the minor arc of this circle with endpoints represented by the triangular libration points represents-when the given primary is excluded-locus of all the points on the Hill's curves that are the least distant points from the given primary. 相似文献
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Dieter Lorenz-Petzold 《Astrophysics and Space Science》1985,109(2):411-411
We wish to point out that the Brans-Dicke-Bianchi type-III vacuum solution recently given by Tiwari and Singh (1984) is not new. Moreover, the solution given has no correct Einstein limit, contrary to what is claimed by these authors. The Ellis-MacCallum vacuum solution in the Einstein case can be obtained from the Brans-Dicke solution first given by Lorenz-Petzold (1984a). 相似文献
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It is shown that the planetary nebulae can be divided into three types according to the values of the mass of shell and a central star. The criteria are given using which one can determine the mass type of the nebula. The distance scale of each mass-type planetary nebulae is given. The distribution of planetary nebulae in the Galaxy, their formation rate, scale-height and other physical and kinematic characteristics are investigated. A catalogue of planetary nebulae emitting in the radio range is given. 相似文献
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Luiz Paulo R. Vaz 《Astrophysics and Space Science》1985,113(2):349-364
The weakest point in the modern models of eclipsing binary systems (EBS) is the treatment given to the effects of mutual irradiation. In this review, which does not have a similar one in the literature, I tried to collect all the work done on the irradiation problem until the middle of 1984, in order to make possible an evaluation of the present status of problem. Special emphasis is given to the applicability of the results to the analysis of EBS. The treatment given to the effect by the early studies as well as by practically all the modern models of EBS is described, and special attention is given to works analysing the problem using stellar model atmospheres. It turns out that the effect is more complex than suspected earlier, but that significant progress has been made recently.Review article. 相似文献
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In the present paper revised distances of optical objects from radio sources of the 5C2 survey are given. A statistical investigation of the data is given for blue objects and galaxies by the statistical method of the “first neighbour”. The identification rate on blue plates for both the blue objects and galaxies amounts to about 40% out of the total number of 26 identifications. For every blue object and galaxy which are proposed as an identification the statistical reliability is given. 相似文献