中国天文学会学术会议(序号:366)2007年学术年会(2007年11月22-25日,广州)

中国天文学会2007年学术年会于2007年11月22-25日在广州召开.会议由中国天文学会主办.广州大学、广东省天文学会承办.包括周又元、方成、陆琰、李惕培、黄润乾等5位院士在内的310多名来自天文界各领域的专家、学者和180多名研究生参加了会议.     

中国天文学会学术会议(序号5):射电天文学术讨论会(1983年9月,北京)

由中国天文学会射电天文专业委员会主持召开的全国射电天文学术会议于一九八三年九月二日至八日在北京大学举行。来自全国有关十一个单位四十一名正式代表参加了会议。中国科学院数理学部副主任、北京天文台台长王绶琯同志,北京大学地球物理系系主任谢炎同志到会讲话,祝贺会议召开。     

中国天文学会学术会议(序号:364):2005年学术年会(2005年10月14～17日,合肥)

中国天文学会2005年学术年会于2005年10月14～17日在中国科学技术大学隆重召开。会议由中国天文学会主办，中国科学技术大学、安徽省天文学会承办。来自全国各天文单位的与会代表共262人，其中既有孜孜不倦为我国天文事业作出重大贡献的老一辈天文学家，也有一批生机勃勃、已作出优秀成绩的青年天文学家。叶叔华、苏定强、陆琰、朱能鸿、李惕碚、方成、周又元等7位院士参加了会议。     

中国天文学会学术会议(序号86):天文仪器与技术第八次学术报告会(1988年11月29日-12日1月,上海)

中国天文学会天文仪器与技术专业委员会第八次学术报告会于一九八八年十一月二十九日至十二月一日在上海召开。会议由专业委员会与上海天文学会共同举办。来自全国十个单位的四十七名代表参加了会议,天文仪器与技术专业委员会主任李德培、副主任龚守身、王传晋和蒋世仰分别主持了报告会。中国天文学会副理长、上海天文台台长叶叔华到会并讲了话。会上宣读了二十四篇论文(见附录及会议资料),其中成     

中国天文学会学术会议(序号12):1984年全国天体测量学术年会(1984年12月,北京)

中国天文学会天文地球动力学和星表与天文常数两个专业委员会于1984年12月3—8日在北京联合举办了天体测量学术年会,参加者有各天文、测地、气象、地震等19个单位的70多名代表。北京天文学会理事长冯克嘉到会讲话,祝贺年会召开。北京天文台台长王绶琯会见了与会代表,表示欢迎。     

中国天文学会学术讨论班1985年序号7:双星(1985年 6月,承德)

全国第二次双星讨论班——双星的观测和理论解释,于1985年6月4日至8日在河北省承德召开。参加会议的有来自全国天文研究单位,高等院校等八个单位的38名代表。中国天文学会副理事长、北京天文台台长王绶琯参加了会议。美国内布拉斯加     

中国天文学会学术会议(序号2):天文地球动力学和星表、天文常数会(1983年4月,武汉)

由中国天文学会天文地球动力学专业委员会和星表与天文常数专业委员会联合举办的1983年学术讨论会,经中国科学院测量与地球物理研究所筹备,于4月24日～26日在武汉召开。参加单位有中国科学院所属各天文台,南京大学和北师大天文系以及测绘部门的代表共76名。中国天文学会副理事长、     

中国天文学会学术会议(序号64):1987年射电天文学术讨论会(1987年9月,上海)

由中国天文学会射电天文专业委员会,上海市天文学会和上海天文台联合举办的“1987年射电天文学术讨论会”于1987年9月1日至3日在上海天文台举行。有来自全国11个单位的代表共39人参加,提交的学术论文报告共51篇。 这次学术讨论会的主要目的是交流近一、二年来射电天文界所取得的研究成果,同时为“亚太会议”的召开进一步作好学术准备工作。提交会议的学术论文报告范围广泛,内容丰富,可分为下列五     

中国天文学会普及委员会1984年工作会议(1984年12月,广州)

1984年12月4日至7日,中国天文学会普及委员会在广州华南师范大学科学技术交流中心召开第四届工作会议。出席本届会议的代表共49名,他们分别来自全国各地方天文学会、天文台、系、厂、馆、出版社和青少年宫(天文部分),还有特邀的科学家和教授等。 会议期间,普及委员会委员陈晓中、杨建、张明昌、沈凯先、李挺等都作了报告。这些报告引起与会者的广泛兴趣。     

中国天文学会首届学术大会(2000年9月21～23日，上海)

中国天文学会首届学术大会于２０００年９月２１～２３日在中国科学院上海天文台召开。这是我国天文界第一次召开这样大规模的综合性学术会议。来自全国各地的１７８名天文工作者参加了这一盛会。会议安排了大会特邀报告、三大组（分太阳与太阳系、恒星与星系、应用天文与仪器三个大组）报告和各专业委员会会议。大会特邀报告共有九个专题。它们分别是：１．宇宙大爆炸学说;２．我国近年来天文的新发现;３．天文在夏商周断代工程中所起的作用;４．γ暴研究新进展;５．星系形成与演化;６．应用天文学研究进展;７．太阳系探索和地外生命…     

Seasonal photometric variability of Titan, 1972–2006

Measurements at Lowell Observatory of Titan in the b (472 nm) and y (551 nm) filters of the Strömgren photometric system at thirty four consecutive apparitions (282 nights) from 1971/72 to 2006 show a 10% sinusoidal variation that lags seasonal extremes by about 1/8 of a Titan year. The seasonal variations are asymmetric: the autumn lightcurve maxima of the northern and southern hemispheres differ significantly as do the spring lightcurve minima. Changes also occur from one Titan year to the next: Titan was ∼3% fainter in b and ∼1% fainter in y following the 2002 southern summer solstice than it was one Titan year earlier in 1973. These changes appear to be intrinsic to Titan's atmosphere and cannot be explained by instrumental effects and changing geometries. Orbital variations visible in recent Hubble Space Telescope images at 673 nm and Voyager orange images (590–640 nm) may have a small (0.002±0.001 mag) counterpart in the b, y photometric record (eastern elongation brighter, consistent with the Cassini near-infrared albedo map).     

Tvashtar awakening detected in April 2006 with OSIRIS at the W.M. Keck Observatory

We detected a volcanic outburst in Io's northern hemisphere on 17 April 2006 with the OSIRIS imaging spectrometer at Keck, and confirmed it was still erupting on 2 June 2006. The eruption, which we name 060417A, was located in Tvashtar Paterae, ∼100 km southeast of the February 2000 eruption. The observed temperature was , over a surface area of , providing a total thermal output of .     

Dynamic of Polar Plumes Observed During 2006, 2008, 2009 and 2010 Total Solar Eclipses

Based on observations of polar plume kinematics in the white-light corona during the total solar eclipse in 2006, the images obtained during multi-station observation of the eclipses of 2006, 2008, 2009 and 2010 were analysed. Several polar plumes showing similar kinematics were identified. The speeds of these dynamic features were found by comparing images obtained at different times along the path of totality. A possible connection with erupting spicules and macrospicules is discussed.     

Observation of Mercury's sodium exosphere during the transit on November 9, 2006

A rare, but normal, astronomical event occurred on November 9th 2006 (JST) as Mercury passed in front of the Sun from the perspective of the Earth. The abundance of the sodium vapor above the planet limb was observed by detecting an excess absorption in the solar sodium line D₁ during this event. The observation was performed with a 10-m spectrograph of Czerny-Turnar system at Domeless Solar Tower Telescope at the Hida Observatory in Japan. The excess absorption was red-shifted by 10 pm relative to the solar line, and was measured at the dawnside (eastside) and duskside (westside) of Mercury. Between the dawn and dusksides, an asymmetry of total sodium abundance was clearly identified. At the dawnside, the total sodium column density was 6.1×10¹⁰ Na atoms/cm², while it was 4.1×10¹⁰ Na atoms/cm² at the duskside. The investigation of dawn-dusk asymmetry of the sodium exosphere of Mercury is a clue to understand the release mechanism of sodium from the surface rock. Our result suggests that a thermal desorption is a main source process for sodium vapor in the vicinity of Mercury.     

The Dark Spot in the atmosphere of Uranus in 2006: Discovery, description, and dynamical simulations

We report the first definitive detection of a discrete dark atmospheric feature on Uranus in 2006 using visible and near-infrared images from the Hubble Space Telescope and the Keck II 10-m telescope. Like Neptune's Great Dark Spots, this Uranus Dark Spot had bright companion features that exhibited considerable variability in brightness and location relative to the Dark Spot. We detected the feature or its bright companions on 16 June (Hubble), 30 July and 1 August (Keck), 23-24 August (Hubble), and 15 October (Keck). The dark feature—detected at latitude ∼28±1° N with an average physical extent of roughly 2° (1300 km) in latitude and 5° (2700 km) in longitude—moved with a nearly constant zonal velocity of , which is roughly 20 m s⁻¹ greater than the average observed speed of bright features at this latitude. The dark feature's contrast and extent varied as a function of wavelength, with largest negative contrast occurring at a surprisingly long wavelength when compared with Neptune's dark features: the Uranus feature was detected out to 1.6 μm with a contrast of −0.07, but it was undetectable at 0.467 μm; the Neptune GDS seen by Voyager exhibited its most prominent contrast of −0.12 at 0.48 μm, and was undetectable longward of 0.7 μm. Computational fluid dynamic simulations of the dark feature on Uranus suggest that structure in the zonal wind profile may be a critical factor in the emergence of large sustained vortices.