共查询到20条相似文献，搜索用时 109 毫秒
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本文给出了大气视宁仪和长焦拖影两种方法，两种仪器在同一圆顶内的同时观测结果及相关分析，结果表明，两种方法所观测到的结果有明显的相关性，相关系数γ＝０．９１。本文还论证了安徽光机所宋正芳等人所研制的大气视宁仪系统是可靠的。 相似文献
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云南天文台丽江高美古和昆明的大气视宁度研究 总被引：5，自引：1，他引：4
研究云南天文台昆明凤凰山和丽江高美古两地点的大气视宁度。利用云南天文台于1994年建立的3孔较差视宁度监视仪（3孔DIMM），对这两个地点的视宁度对比观测。还利用云南天文台的1米望远镜所得到的视宁度与3孔DIMM所测的视宁度进行对比。1米望远镜和3孔DIMM同时观测了7个晚上，各取得308组数据，它们的视宁度平均分别为0．90〃和0．84〃。还讨论了3孔DIMM采用不同曝光时间对视宁度测量值的影响，从实验得出3孔DIMM采用20ms曝光比采用8ms曝光所测视宁度的值要好15％左右。从1995年5月－1996年12月，对丽江高美古和昆明凤凰山二地进行了视宁度的对比观测。在高美古和昆明分别观测了234夜和256夜，观测结果是两个点的视宁度平均；丽江为0．70〃，昆明为0．95〃，同时也统计了两个点的月平均视宁度和最好夜的视宁度，并讨论了两地视宁度随时间的变化规律。 相似文献
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差分像运动视宁度测量实验 总被引：1，自引：0，他引：1
本文首先阐明了Ｆｒｉｅｄ参数（大气相干长度）ｒ０的物理含义及为什么选取ｒ０作为表征大气视宁度的参数；然后介绍了一种优良的测量ｒ０的方法－差分像运动法，总结了该方法的六个特点，最后给出了在云南天文台用该方法的六个特点，最后给出了在云南天文台用该方法两次实测大气视宁度的实验结果及实验参数，并对结果进行了分析。 相似文献
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用1979—1980年食期间观测的11夜光谱底片,以做(Δλ)/(Δx)～λ色散曲线的方法,得出了ζAur的视向速度随位相的变化。其结果列于表2,绘于图1。 同以前食期间得到的视向速度相比较,结果基本一致,但在即将全食的大气食期间所得到的视向速度明显偏低。本文对这些结果做了初步讨论。 相似文献
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本文初步对比分析了昆明大气探空资料与大气视宁度观测资料之间的相关关系。结果表明，它们之间有着明显的关系和规律，但关系式的确立还需更多的资料分析才能确定。 相似文献
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介绍了丽江高美古二期选址的筛选工作，经过踏勘确定高美古周围山头的10个点为筛选点，采用小型轻便望远镜于1998年10月16至1999年1月27日进行目视衍射环观测，并对取得的资料作了处理、分析和初步探讨。观测发现各点的视宁度没有明显差别，6 相似文献
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讨论了经过大气后天文图象的象质衰减,研究了对这种衰减进行描述的视宁度参数ｒ０及其它几个大气光学参数,介绍了几种测量象质衰减参数的方法,重点介绍了我们将差分像运动法运用于白日视宁度测量的尝试以及新设计的可兼顾昼夜的视宁度测量仪,仪器已用于云台白日的视宁度测量。最后对近场近似假设进行了定量分析,在此基础上给出了新确定的近场近似成立的范围,这一范围比以前所给的要更大些。 相似文献
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介绍了丽江高美古二期选址在踏勘和筛选工作的基础上 ,对 3 # 点和6# 点的视宁度进行了对比观测。通过对 1 999年 2月 6日～ 1 999年 1 2月 3 1日 2个点共 4 756组同时段观测数据的统计和处理得到 :3 # 点的视宁度平均值为 1 1 .2 62 3cm ,6# 点的视宁度平均值为 1 1 .5952cm。经F分布检验和t分布检验假设成立 ,作出 3 # 点和 6# 点的视宁度无显著性差异的推断 ,与初期用衍射环观测视宁度的结果一致 ,进一步说明了高美古整个山头的视宁度都是优良的 相似文献
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Various methods for measuring areas of sunspots and umbrae are compared to test their robustness against changing seeing conditions. The influence of the seeing is simulated by artificially degrading high-resolution sunspot images. A new procedure – the so-called inflexion point method – for area determinations is described. It is based on the calculation of the inflexion point contours of the two-dimensional sunspot intensity distribution. The areas derived with this method are much more stable against seeing influences than those obtained by the other procedures tested. The effect of the seeing on the measurements of the bolometric sunspot contrast and irradiance deficit produced by a sunspot is also studied. 相似文献
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据近二年的实地观测结果说明丽江高美古处在我国南方晴夜较多的地区且具有极好的视宁度。作者建议放置一台６０ｃｍ口径的望远镜进行天文观测并进一步证实该地的视宁度质量。 相似文献
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Pei Chong Yuan Xiang-Yan Chen Hua-Lin Zhao Jian-Lin WEN Hai-Kun Li Zheng-Yang 《Chinese Astronomy and Astrophysics》2012
The Antarctic site-testing campaigns have shown that Dome C is an excellent astronomical site on the earth, it is better than any of existing mid-latitude astronomical sites in the world, because of its cold and dry weather, low infrared background radiation, continuously observable time as long as 3–4 months, clear and highly transparent atmosphere, low wind speed, and the absence of dust and light pollution. And in the international astronomical community it is generally believed that Dome A with a higher altitude may be better than Dome C as a potential excellent astronomical site. In the past 3 years, although held by the Center for Antarctic Astronomy of Chinese Academy of Sciences, the site testing at Dome A has preliminarily con?rmed the many advantages of Dome A as an excellent astronomical site, but the data about the atmospheric seeing, which is an important parameter for assessing the site quality for optical observations, have not been obtained until now. Hence, on the basis of a commercial telescope with the diameter of 35 cm, we have made the hardware reformation and software development to have it operate as a DIMM (Differential Image Motion Monitor), which can simultaneously monitor both the seeing and isoplanatic angle at Dome A automatically. At present this instrument has been shipped to Antarctica by the “Xuelong” exploration ship, and will be installed at Dome A, and begin to work in early 2011. Before the shipment, by through the comparative measurements together with an existing seeing monitor at the Xinglong astronomical station, the software, hardware, as well as the installation and adjustment of the instrument, are further veri?ed by testing. 相似文献
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S. Djorgovski 《Journal of Astrophysics and Astronomy》1983,4(4):271-288
Convolution methods for modelling of astronomical seeing effects have been investigated. The advantages and disadvantages
of several techniques are discussed, and particular attention is given to the fast Fourier transform (FFT) method. This method
is then applied to two classes of problems, the structure of cores of elliptical galaxies, appearance of distant galaxies
and the consequences of seeing effects in some cosmological tests. Estimates are presented for dimming of the central surface
brightness and changes in the apparent core radius for elliptical galaxies, as well as seeing-induced changes in ellipticity.
Modelling of galaxies with stellar nuclei has also been performed. Some consequences of these effects in investigations of
dynamics of elliptical galaxies are addressed briefly. The influence of seeing in observational cosmology is discussed in
the context of Hubble diagram (m-z) tests. It is shown that inadequate compensation for seeing effects can seriously distort the conclusions in such tests.
Some suggestions for future work in this direction are offered. 相似文献