共查询到19条相似文献，搜索用时 193 毫秒
1.
对文[2]的4颗流量标准星HD19445、HD84937、BD 17°4708和BD 26°2606中的2颗:HD19445和HD84937所在天区,用BATC15色测光系统中的14色滤光片(除b片外)进行测光。利用批处理程序PipelineI和PipelineⅡ对观测数据进行处理,并利用观测天区中标准星已知的BATC星等来确定天区内的其它恒星的BATC星等。我们估算出天光背景值,并寻找得到的信噪比与BATC星等mbatc以及曝光时间t之间的关系,最后得到三者之间的经验关系公式。 相似文献
2.
狐狸座PU是1979年4月8日由日本东京天文台Y.Kuwano等人首先发现的一颗光度变化特殊的类新星天体.1978—79年间,梅苞在用北京天文台40/200双筒天体照相仪对这一天区的其他天体作系统观测时,同时取得了这颗星的一批照相观测资料,在获悉有关这颗星的发现报道之前,他也曾独立地发现了这颗星的光度变化(图版Ⅰ,图2),并随即用北京天文台的60/90/1800施密特望远镜有缝摄谱仪取得了该星的部分光谱资料.此外,还用北京天文台60厘米反射望远镜进行了高速光电观测.从1978年12月到1983年3月,共取得照相观测底片和光谱片200余张以及一些光电测光资料. 相似文献
3.
本文对RZ Dra 1978年的光电光变曲线,重新用Wilson-Devinney综合光变曲线分析程序进行了测光解,新解表明Rz Dra是一颗半相接双星,质量较小的次子星充满临界等位面,而质量较大的主子星接近充满其临界等位面.两子星的测光质比q=0.664.从而得到系统的绝对参量,并讨论了它的演化阶段.系统可能存在着主要通过拉格朗日L_2点的物质流失,从而引起观测到的轨道周期缓慢减小的变化. 相似文献
4.
对29颗Be星作了近红外JHK宽波段测光。所选对象多少有些特殊性。其中19颗有或可能有快周期光变,6颗是Be/x射线双星。观测用光学天文开放实验室北台兴隆站1.26米红外望远镜。观测结果表明相当多的星有较大的红外超,其中8颗星的J-K值大于0.5;有3颗星有较明显变化,△(J-K)大于0.4。 相似文献
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6.
谭徽松 《中国天文和天体物理学报》1986,(2)
用美国McDonald天文台2.1米反射镜的折轴Reticon观测HeI 5875谱线,由标准星的观测轮廓与Gray的转致轮廓卷积后同被测星的观测轮廓进行拟合,测得了18颗双星的Vsini,并结合以前测得的20个双星系统的结果,同Slettebak老系统进行了比较,得到了它们的近似关系:在Vsini<100 kms~(-1)时,两者的值比较一致;当Vsini>100kms~(-1)时,本方法得出的值明显偏低。这一关系间接说明,我们的结果与Slettebak新系统的趋势是一致的。 相似文献
7.
黑洞暂现双星MAXI J1820+070于2018年3月的明亮爆发为研究光学快速测光能力提供了重要机遇. 以快速光学相机(Fast Optical Camera, FOC)为终端设备分别在2018年4月22日、5月26日和8月31日(UTC)使用云南天文台丽江观测站2.4m望远镜对爆发中的黑洞双星MAXI J1820+070进行了亚秒时标的测光观测. 通过观测数据分析, 研究了相机的快速测光性能.对全帧和1/4帧两种观测模式的帧间间隔(frame time), 测得平均帧间间隔为(22.866 pm 0.679)ms和(5.868 pm 0.169)ms. 通过视场中多颗明亮参考源校准,提取了观测对象和参考源的光变曲线, 获得了光变曲线的傅里叶功率谱, 区分了观测对象本征光变和仪器或望远镜等观测因素带来的非本征光变, 成功探测到目标黑洞双星MAXI J1820+070中的光学波段低频准周期振荡信号, 并判别了观测中来自仪器设备或与观测条件相关的时变信号. 这成功验证了相机高速稳定的测光性能和对短至5ms时标光变信号的探测能力. 相似文献
8.
用相同的仪器条件在美国基特峰国立天文台观测了１２颗晚型双星，并用卷积法测得了这１２个双星系统的１５个子星的自转速度，其中５个子星是首次进行自转测量。利用我们自己测得的自转速度值，我们也讨论了这些双星系统中的自转同步性。结果显示：所有轨道周期小于９天的双星系统子星都是周步自转的 相似文献
9.
我们用美国McDonald天文台2.1米反光镜Coude Reticon观测,对31个RS CVn型双星系统的37颗子星的自转进行了测量。并结合以前测得的38颗子星的数据,对RS CVn型星是否同步作了统计分析,结果表明,绝大多数都显示出同步自转性质;但无论是短周期、正常周期还是长周期组的,都有少数与同步自转不一致的例子。这与过去认为短周期和正常周期的呈同步自转,而长周期的呈非同步自转的结论不一致。 相似文献
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对北京天文台新近改造成的三通道高速光度计的结构和性能进行介绍,并给出了在兴隆站85公分望远镜的一些实测结果. 相似文献
12.
The eclipsing binary V392 Ori was observed photoelectrically, from November 1984 to January 1985, inUBV bands using the P34B photometer attached to the 0.91 m reflector at the McDonald Observatory. Four-hundred eighty-six observations in each band were obtained. Six primary and 4 secondary minimum were observed during this period. The light curves show a typical Beta Lyrae-type variation instead of an Algol-type light curve reported earlier. 相似文献
13.
Two events of outburst of Garnet Hale - Bopp occurred on Oct. 9,1996 and Nov. 13,1996 are observed by means of photoelectric integrating photometer mounted on the 60cm reflector of Purple Mountain Observatory. The results are shown in Tab. 3, Fig. 1 (Oct. 9, 1996) and in Tab.4,Fig.2(Nov.13,1996). 相似文献
14.
Yang Tinggao 《时间频率学报》1995,(1)
根据对鬼星团中Ｊｏｈｎｓｏｎ测光标准星的观测，我们研究了北京天文台６０ｃｍ望远镜直流光电光度计ＵＢＶ测光系统的转换方程．应用该方程推算了对三颗变星观测得到的ＵＢＶ星等，讨论了所得光变曲线的精度，并与较差方法所得结果进行了比较 相似文献
15.
The search of roAp stars at Mt. Dushak-Erekdag Observatory was started in 1992 using the 0.8 m Odessa telescope equipped with
a two-star high-speed photometer. We have observed more than a dozen stars so far and discovered HD 99563 as roAp star while
BD+8087 is suspected to have rapid oscillations. Negative results of our observations for the search of rapid oscillations
in four stars in NGC 752 are also discussed. 相似文献
16.
We designed a prime focus CCD photometer, Argos, optimized for high speed time-series measurements of blue variables (Nather
& Mukadam 2004) for the 2.1 m telescope at McDonald Observatory. Lack of any intervening optics between the primary mirror
and the CCD makes the instrument highly efficient. We measure an improvement in sensitivity by a factor of nine over the 3-channel
PMT photometers used on the same telescope and for the same exposure time. The CCD frame transfer operation triggered by GPS
synchronized pulses serves as an electronic shutter for the photometer. This minimizes the dead time between exposures, but
more importantly, allows a precise control of the start and duration of the exposure. We expect the uncertainty in our timing
to be less than 100μs.
Hubble Fellow 相似文献
17.
使用1994—2007年在1．56m反射望远镜CCD照相机拍摄的资料，测定了上海天文台余山工作站夜天亮度的变化。由于上海城市的发展，佘山工作站的夜天亮度在V波段从每平方角秒约19mag变到15．8mag，也就是说，夜天亮度自1994年以来变亮了约20倍。国际上优良台站的夜天亮度在V波段等于或暗于21．5mag。上述夜天亮度是优良台站的200多倍。现在在佘山工作站使用1．56m反射望远镜对暗于V=14mag的星做精确测光已经很困难了。 相似文献
18.
David S. Evans 《Earth, Moon, and Planets》1973,8(4):490-499
Since 1968 an assiduous program of photoelectric observation of occultations of stars by the Moon has been pursued at McDonald Observatory. A total of about 600 events has been observed of which 254 have been published and a second list is in preparation. Timings derived from the reductions have errors of the order of 1 ms corresponding to a positional uncertainty in the lunar limb of typically 80 cm. Results are routinely communicated to the ephemerides offices.In about 140 events the fringe pattern due to diffraction by the lunar limb is sufficiently well defined to permit a determination of the slope near the point of occultation. A statistical discussion of these data is given. In all except a few cases, the slopes are numerically less than 15°, though 7 cases with slopes between 30° and 40° have been found. The relations between numbers of observations and contact angle, and between errors of slope determination and contact angle are discussed. The distribution of slope data with contact angle seems adequately explained. When slope data are collected by position angle consistently large and consistently small values show a tendency to group in a pattern suggesting a connection with observed large scale features on the lunar limb.The influence of lunar limb irregularities of a scale of a few meters on observed diffraction patterns and inferred timings is discussed. Multichannel observations should be of value in removing ambiguities. The use of occultation observations for the discovery of multiple stars and for the measurement of angular diameters of stars is mentioned. Future developments proposed for the project are considered.The project has involved contributions by a considerable number of individuals from the staff and student body at Austin, Texas, from the staff at McDonald Observatory, from visiting scientists and from the Laser Ranging Group. These contributions are acknowledged in the paper. The work has been supported by NSF Grants GP-21204 and GP-32263X.Communication presented at the conference on Lunar Dynamics and Observational Coordinate Systems held January 15–17, 1973 at the Lunar Science Institute, Houston, Tex., U.S.A. 相似文献
19.
Differential BVR photometric observations of the three RS CVn binary stars: V711 Tau, UX Ari and IM Peg obtained during the period November 26, 1994–February 24, 1995 using the 0.35 m reflector telescope equipped with photoelectric photometer are presented. Analysis of light curves shows significant changes in shape, amplitude as well as the phases of minimum light of all the three binaries. The amplitude of IM Peg, in particular, is found to have reached a larger value in the present epoch of observation than reported earlier. 相似文献