天文学进展第20卷2002年总目录

如何写好天文学论文….…………………………………………Helmut A.Abt(4,299)天文学、天文学史光污染和光学天文台址保护…….…………………………………..谭徽松岑学奋(1, 1)虚拟天文台的技术进展………………………………崔辰州赵永恒赵刚张彦1|【(4,302)天文学中的数据挖掘和知识发现 ……….…………….……..张彦厦赵永恒崔辰州(4,312) 仪器与技术国外原子时频最新进展……………………………….……………潘蜂翟造成(3,201)方位天文、天体力学相对论框架中的时间计量………………………………………………….韩春好(2,107)GPS掩…     

光学天文台址的高度探讨

本文对全球现有天文台址的海拔高度、大望远镜所在地的高度和近十年来的光学天文台的选址在海拔高度上的考虑进行了综述和分析,并对云南境内候选点的高度提出看法。     

丽江高美古的天文观测条件

综述对丽江高美古的视宁度、天光亮度、消光系数进行观测的原理、仪器、观测方法和结果．结果表明,高美古是我国南方的优良光学天文台址,视宁度达到世界优良台址的水平     

南极冰穹A首台自动视宁度检测仪的研制

南极冰穹C (Dome C)的选址结果显示:Dome C具有寒冷干燥、红外背景辐射低、可连续3～4个月观测、空气明净、透过率高、风速低等特征,是比地面上任何中纬度台址都好的天文观测台址.而由我国最先登陆的内陆最高点冰穹A (Dome A)被国际天文界广泛认为可能是比Dome C更好的天文台址.近3 yr来,中国科学院南极天文中心领导开展Dome A的台址测量工作,初步结果表明Dome A作为天文台址具有巨大优势.但是到目前还没有获得直接用于衡量天文台址在光学观测方面的主要参数—视宁度数据.介绍了中国科学院南京天文光学技术研究所自行研制的我国首个用于Dome A的自动视宁度测量仪,基于一台口径35 cm的商用望远镜进行硬件改造和软件开发,使其能在Dome A低温低压环境下进行自动观测和数据处理.目前该仪器已随“雪龙号,科考船起运南极,于2011年初安装到Dome A并开始测量.起运前,在兴隆观测站与中国科学院国家天文台(国台)选址组的一台视宁度监测仪进行了对比测量,对软件、硬件和装调方法进行了检验验证.     

基于ASCOM及PLC的随动天文圆顶控制

四川稻城县无名山址点是云南天文台新近选定的天文台址。为实现在无名山50 cm光学望远镜开展远程自动观测,需要对圆顶进行远程自动控制驱动开发。基于天文公共对象模型(Astronomy Common Object Model, ASCOM)标准,采用Modbus/TCP协议连接可编程控制器(Programable Logical Controller, PLC),实现了圆顶的自动控制。重点介绍了圆顶控制原理和实现方法,结果表明,圆顶控制系统具有融合度高、使用方便的特点,满足远程自动观测的需求,对于中小型观测系统具有一定的借鉴意义。     

天文台址资源调研专家组第五次会议纪要

天文台址资源调研专家组第五次会议纪要天文台址资源调研专家组第五次会议于１９９５年８月１１—１２日在云南天文台召开。参加会议的有专家组成员张柏荣、苏洪钧、谭徽松、胡景耀、侯金良、黄寅亮，专家组成员韩博因事未出席会议。应邀参加会议的还有陈建生、苗永瑞、郝...     

天文台址资源调研专家组1996年第2次会议纪要

天文台址资源调研专家组１９９６年第２次会议纪要根据天文台址资源专家组１９９６年第１次会议纪要精神，本年度第２次会议的第一部份于７月１９－７月２０日在昆明召开。论证了在高美古进行微温测量、将ＤＩＭＭ观测抬高到１０ｍ高度进行，将ｏｃｍ望远镜移到高美古进行...     

丽江高美古的大气消光系数测定

１９９６年１－２月，我们用光电方法测定了丽江高美古在Ｂ、Ｖ两个波段的大气消光系数。为便于比较，在同一时期还测定了云南天文台凤凰山台址的大气消光系数。本文给出了观测结果，同时也列出了世界上一些天文台站的数据以供参考。     

大气光学湍流模型计算方法

光学湍流的强弱和分布是描述天文台址优劣的重要参数.介绍了利用大气模式WRF (Weather Research and Forecasting Model)计算高美古站周围大气光学湍流参数的方法,这些参数包括C2n(大气光学湍流强度)廓线、大气相干长度、大气相干时间、视宁度、等晕角和闪烁率等.包括模型计算方法的实现过程、模型的设置和模拟结果的验证.计算结果与云南高美古观测站DIMM (Differential Image Motion Monitor)的实测数据进行了对比.     

凤凰山的今昔

凤凰山天文台原是抗日战争时期中央研究院天文研究所的临时所址。我在那里度过了七、八个寒暑。当年的凤凰山天文台现在已成为我国天文机构中建设规模最为宏大的云南天文台大本营的所在。一年前旧地重临,目睹今昔的巨大变化,恍如隔世。回忆往事,感触很多。     

中国出口双折射滤光器

中国科学院南京天文仪器研制中心在20世纪80年代研制35cm太阳磁场望远镜滤光器取得巨大的成功，其在双折射滤光器领域内的水平，已被国际太阳物理界公认。1989年以来，已向日本和韩国出口了11台复杂而昂贵的Lyot滤光器，并已在有关国立天文台和天文馆投入常规观测。最近，还为国外客户修复3台Lyot滤光器，它们都是德国和法国在30年前生产的。     

Intercalibration of airglow observatories with the atmosphere explorer satellite

The visible airglow photometer on the Atmosphere Explorer C Satellite has been used to compare the calibrations of a number of ground-based airglow observatories. Discrepancies between different ground stations as large as a factor of six have been revealed. Efforts to account for these discrepancies have resulted in the discovery of differences as large as a factor of 2 in the standard light sources in use at different observatories. The participation of additional observatories in the intercomparison of standard sources is solicited. The project has also led to the discovery of a source of error that can amount to another factor of 2 in the procedure used to calibrate many airglow instruments. In the course of the project detailed maps, based on satellite data, have been made of the galactic and zodiacal light background at a number of wavelengths, and a substantial source of contaminating emission has been discovered in the satellite data; the contamination appears to result from interaction of the spacecraft and the atmosphere at altitudes below 170 km.     

Photoelectric photometry of the RS CVn binary EI Eridani = HD 26337

DifferentialUBV(RI) _KC andUBVRI photometry of the RS CVn binary EI Eridani obtained during December 1987 and January 1988 at fourteen different observatories is presented. A combined visual bandpass light curve, corrected for systematic errors of different observatories, utilizes the photometric period of 1.945 days to produce useful results. Analysis shows the visual light curve to have twin maxima, separated by about 0.4 phase, and a full amplitude of approximately 0.06 mag for the period of observation, a smaller amplitude than reported in the past. The decrease in amplitude may be due to a decrease or homogenization of spot coverage. To fit the asymmetrical light curve, a starspot model would have to employ at least two spotted regions separated in longitude.     

Preliminary Photometric Results for the 2003 Eclipse of Ee Cep

We report multicolour photometric observations of the 2003 eclipse of the long-period (5.6 yr) eclipsing binary EE Cep. Measurements were obtained with ten telescopes at eight observatories in four countries. In most cases, UBV(RI)_C broad band filters have been used. The light curve shape shows that the obscuring body is an almost dark disk around a low-luminosity central object. However, variations of the colour indices during the eclipse indicate that the obscuring body emits a considerable amount of radiation in the near infrared.     

Light Pollution and its Energy Loss

Data obtained by US DMSP satellites were analyzed to obtain light energyin order to monitor light pollution at different countries. Light detectedby the satellites is one ejected to space and is not mostly used toilluminate objects to be seen. This light is energy loss and produce lightpollution for astronomical observation. We should reduce such energy lossand light pollution.     

Backyard spectroscopy and photometry of Titan, Uranus and Neptune

We present and discuss observations of Titan (photometry and spectroscopy) and Uranus and Neptune (spectroscopy only) obtained using off-the-shelf equipment, affordable and available to many amateur astronomers and small colleges. Spectral observations compare well with published results from front-line observatories, and some evidence of seasonal change is evident in both spectra and narrowband photometry. Scattered Saturn light presents a significant problem for Titan observations, in particular, for slitless spectroscopy, and our attempts to reproduce Titan's lightcurve have so far been unsuccessful.     

How to build a continental scale fireball camera network

The expansion of the Australian Desert Fireball Network has been enabled by the development of a new digital fireball observatory based around a consumer digital camera. The observatories are more practical and much more cost effective than previous solutions whilst retaining high imaging performance. This was made possible through a flexible concurrent design approach, a careful focus on design for manufacture and assembly, and by considering installation and maintenance early in the design process. A new timing technique for long exposure fireball observatories was also developed to remove the need for a separate timing subsystem and data integration from multiple instruments. A liquid crystal shutter is used to modulate light transmittance during the long exposure which embeds a timecode into the fireball images for determining fireball arrival times and velocities. Using these observatories, the Desert Fireball Network has expanded to cover approximately 2.5 million square kilometres (around one third of Australia). The observatory and network design has been validated via the recovery of the Murrili Meteorite in South Australia through a systematic search at the end of 2015 and the calculation of a pre-atmospheric entry orbit. This article presents an overview of the design, implementation and performance of the new fireball observatories.     

埃文斯目视日晕光度计测量原理研究

埃文斯目视日晕光度计（Evans Visual Sky Photometer,EVSP）是应用于日冕仪选址的重要仪器,从20世纪40年代一直使用至今,它为现代日晕光度计的定标提供了参考标准。通过使用云南天文台现存的一架EVSP研究了它的工作原理,并重点介绍了所利用的简易定标方法。给出了国际现有的多台EVSP日晕亮度定标曲线。由于EVSP内部光学元件反射率和透过率,以及中性渐变光楔的光学密度等存在未知的时间缓变特点,因此利用这种新定标手段可以高效经济地获得各自的定标曲线。     

The mean magnetic field of the Sun: Method of observation and relation to the interplanetary magnetic field

The mean solar magnetic field as measured in integrated light has been observed since 1968. Since 1970 it has been observed both at Hale Observatories and at the Crimean Astrophysical Observatory. The observing procedures at both observatories and their implications for mean field measurements are discussed. A comparison of the two sets of daily observations shows that similar results are obtained at both observatories. A comparison of the mean field with the interplanetary magnetic polarity shows that the IMF sector structure has the same pattern as the mean field polarity.