共查询到20条相似文献，搜索用时 156 毫秒
1.
2.
根据１９９４年６月—１９９５年１２月期间在新疆天山南坡的奎先达坂进行的云量观测结果和邻近的巴仑台气象站的多年气候观测资料作统计分析，作者推断奎先达坂的天文可用小时数和天文夜数均可与目前世界上最优良的天文台址相比。 相似文献
3.
4.
5.
6.
收集了我国１９７８─１９８６年和１９９０年，共１０年时间的１９２个地面气象站每天四次总云量的观测资料，分别计算了北京时间０８ｈ，０２ｈ和０８ｈ以及２０ｈ，０２ｈ和０８ｈ的无云概率。分析结果表明：我国所处的天文气候条件的大环境并非是世界上最好的，但在国内相对较好的区域里，精心挑选出受局部地形影响形成的较好台址还是有可能的。 相似文献
7.
8.
我国天文气候特点及潜在（光学／红外）优良台址探讨 总被引：5，自引：0，他引：5
收集了我国１９７８－１９８６年和１９９０年，共１０年时间的１９２个地面气象站每天四次总云量的观测资料，分别计算了北京时间０８ｈ，０２ｈ和０８ｈ以及２０ｈ，０２ｈ和０８ｈ的无云概率，分析结果表明：我国所处的天文气候条件的大环境并非是世界上最好的，但在国内相对较好的区域里，精心挑同受叶形得影响形成的较好台址还是有可能的。 相似文献
9.
经纬天地
为了更好地说明本方法的有效性,笔者选择了一个在地图上很明显的地方,同时又不挨着经纬线的地点——山东半岛最东端成山角的成山头气象站观测场（WMO站号54776,东经122．7032度,北纬37．3951度）来进行演示。 相似文献
10.
11.
统计了全国２３９个气象台站的云量和扬沙天数资料，说明云量较少的地区多分布于内蒙、西藏、甘肃、新疆、宁夏等省、自治区，但在西北地区扬沙天气较多。 相似文献
12.
云南-香港宽视场巡天新发现了一个磁活动双星系统,其轨道周期为0.60286 d.利用云南天文台1 m光学望远镜附加CCD (Charge-Coupled Device)相机,观测得到了这个双星系统的V、Rc双色光变曲线,结果表明该系统食外存在明显的测光畸变.借助云南天文台丽江2.4 m望远镜附加云南暗弱天体光谱成像仪(Yunnan Faint Object Spectrograph and Camera, YFOSC)对该双星系统的分光观测,测定了该双星系统主星的视向速度曲线并发现该系统的主星表面存在着强烈的色球活动,从而证明系统的光变曲线畸变源自主星的黑子活动.使用W-D (Wilson-Devinney)程序分析上述观测得到的光变曲线和视向速度曲线,得到了该双星系统的轨道参数以及黑子参数.最后,对该系统的特性进行了讨论并对未来的工作进行了展望. 相似文献
13.
WANG Jian-hua GU Sheng-hong WANG Xiao-bin Bill YEUNG Eric NG 《Chinese Astronomy and Astrophysics》2021,45(1):67-81
We present a newly discovered magnetically active binary system detected by Yunnan-Hong Kong wide field survey, with an orbital period of 0.60286 days. Two color photometry for the system was performed using the 1 m Cassegrain telescope of Yunnan Observatories with its CCD (Charge-Coupled Device) camera. In the observed light curves, there are clearly different light maxima existed in the out-of-eclipse regions. We made spectroscopic observations for the binary system using the 2.4 m telescope and YFOSC (Yunnan Faint Object Spectrograph and Camera) of Lijiang station of Yunnan Observatories, China. The radial velocity curve was derived for primary star of the binary system. The primary star exhibited strong chromospheric activity, which confirms that the distortion of the light curves results from the starspot activity on the primary star. Through analyzing the light curves and RV (Radial Velocity) curve mentioned above by means of the W-D (Wilson-Devinney) code, orbital parameters and starspot configuration of the binary system are obtained. Finally, we have discussed the properties of the binary system, and given the prospects on the future work. 相似文献
14.
The cosmic-ray (CR) time series were compared with the green 530.3 nm coronal emission line intensity over the period 1951–2003.
There is a clear asymmetry in the cross-correlation between the cosmic rays and green emission corona for the even- and odd-numbered
solar cycles, where a time lag is ranging between 0 and 380 days. While over the period 1954–1964 and 1978–1985 the time lag
is above 200 days, over the period 1965–1976 and 1986–1995 the time lag is below 130 days. A possible reason for the lag asymmetry
is discussed. The cross-correlations between the cosmic rays and Wolf sunspot number over the period 1951–2003 is also presented. 相似文献
15.
16.
L. Valenziano 《Experimental Astronomy》1995,6(1-2):83-96
A valuable seeing estimation at Baia Terra Nova, Antarctica is deduced from meterological data by means of a model. A sounding balloon launching campaign was conducted during the late spring 1993 and summer 1993–94. Using certain assumptions seeing is estimated in daytime and spring-summer conditions. The results obtained can be considered as worst case ones and are discussed as a first step to future programs for astronomy in Antarctica. 相似文献
17.
18.
19.
W. Henze Jr E. Tandberg-Hanssen M. J. Hagyard B. E. Woodgate R. A. Shine J. M. Beckers M. Bruner J. B. Gurman C. L. Hyder E. A. West 《Solar physics》1982,81(2):231-244
The Ultraviolet Spectrometer and Polarimeter on the Solar Maximum Mission spacecraft has observed for the first time the longitudinal component of the magnetic field by means of the Zeeman effect in the transition region above a sunspot. The data presented here were obtained on three days in one sunspot, have spatial resolutions of 10 arc sec and 3 arc sec, and yield maximum field strengths greater than 1000 G above the umbrae in the spot. The method of analysis, including a line-width calibration feature used during some of the observations, is described in some detail in an appendix; the line width is required for the determination of the longitudinal magnetic field from the observed circular polarization.The transition region data for one day are compared with photospheric magnetograms from the Marshall Space Flight Center. Vertical gradients of the magnetic field are computed from the two sets of data; the maximum gradients of 0.41 to 0.62 G km–1 occur above the umbra and agree with or are smaller than values observed previously in the photosphere and low chromosphere. 相似文献
20.
The metric spectral data obtained at the Yunnan Observatory from July 1990 to December 1991 are analysed and some type III bursts associated with millisecond spikes are found. Their different morphologies reveal the relation between the type III bursts and the millisecond spikes. Based on the occurrence time and the characteristics of continuity and changes of the morphologies in the spikes and the type III bursts of two typical events, we verify that the acceleration region of the coronal electrons is located above the emitting region of the millisecond spikes and the type III bursts. The observations show that the interface frequency of a pair of type III bursts lies near 250 MHz. Finally the authors attempt to explain qualitatively the generating mechanism of the metric millisecond spike-type III bursts by means of the plasma hypothesis. 相似文献