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Information Bulletin on Variable Stars最新文献

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NY Her: possible discovery of negative superhumps NY Her:负超凸点的可能发现
Q4 Physics and Astronomy Pub Date : 2017-09-25 DOI: 10.22444/IBVS.6216
A. Sosnovskij, E. Pavlenko, N. Pit, K. Antoniuk
We presents result of CDD photometry for SU UMa dwarf nova NY Her during 6 nights in June 2017 when object was in quiescence. Light curves clearly show strong amplitude variations in a range of 0m.7-1m.1. Time series analysis revealed a period 0.07141(5) d, that we identified as the period of possible negative superhumps of NY Her.
本文报道了2017年6月6夜对SU UMa矮新星NY Her的CDD光度测量结果。光曲线在0m.7 ~ 1m.1范围内明显表现出强烈的振幅变化。时间序列分析显示了0.07141(5)d的周期,我们认为这是NY Her可能的阴性超峰期。
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引用次数: 1
Times of Minima of Some Eclipsing Binaries 某些食双星的极小值时间
Q4 Physics and Astronomy Pub Date : 2017-09-07 DOI: 10.22444/IBVS.6209
E. Bahar, O. Yörükoǧlu, E. M. Esmer, T. Kılıçoğlu, D. Öztürk, M. B. Doğruel, D. Ozuyar, D. Gümüş, D. D. Izci, B. Keten, C. T. Tezcan, H. V. Şenavcı, M. Yılmaz, Ö. Baştürk, S. Selam, F. Ekmekçi, B. Albayrak, S. Caliskan, A. Akcar
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引用次数: 2
Discovery of short-period oscillations in the mass-accreting component of TT Vel TT Vel质量吸积组件中短周期振荡的发现
Q4 Physics and Astronomy Pub Date : 2017-09-07 DOI: 10.22444/IBVS.6238
D. Mkrtichian, K. Gunsriwiwat, D. Reichart, J. Haislip, V. Kouprianov, S. Poshyachinda
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引用次数: 1
SS Cancri: the shortest modulation-period Blazhko RR Lyrae. 巨蟹座SS:调制周期最短的Blazhko RR天琴座。
Q4 Physics and Astronomy Pub Date : 2017-08-10 DOI: 10.22444/IBVS.6213
C. Cafolla, R. Mathew, A. Edge, A. M. Swinbank, G. Lansbury, R. Wilson, T. Butterley, J. Lucey, L. Hardy, S. Littlefair, V. Dhillon
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全文可以和/或复制使用,并给第三方以任何形式或媒介,未经许可或电荷,为个人研究或研究,教育,或not-for-pro t目的提供:•一个完整的书目指的是原始源•链接是由元数据记录在滴•全文并不以任何方式改变了全文不得在任何形式或媒介销售没有正式版权所有者的许可。有关详细信息,请参阅完整的DRO政策。
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引用次数: 0
Spectroscopy of bright Algol-type semi-detached close binary system HU Tauri (HR 1471) 亮algol型半分离紧密双星系统HU Tauri (HR 1471)的光谱学
Q4 Physics and Astronomy Pub Date : 2017-07-20 DOI: 10.22444/IBVS.6233
M. Parthasarathy
Spectroscopic results of HU Tauri that I presented in my Ph.D thesis (Parthasarathy 1979) are published in this paper. The H-alpha line of the secondary is detected. The detection of H-alpha line of the secondary is confirmed based on the high resolution Coude Reticon spectra obtained with the 2.1-m telescope of the McDonald observatory.
本文发表了我在1979年发表的博士论文(Parthasarathy)中对胡的光谱结果。检测到次级的H-alpha线。根据麦克唐纳天文台2.1米望远镜获得的高分辨率Coude Reticon光谱,证实了次级的H-alpha线的探测。
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引用次数: 0
Mass and Precession of the Disk in {zeta} Tau {zeta} Tau星盘的质量和进动
Q4 Physics and Astronomy Pub Date : 2017-07-18 DOI: 10.22444/ibvs.6208
E. Pollmann
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引用次数: 0
New CCD Times of Minima of 17 Eccentric Eclipsing Binary Systems 17个偏心食双星系统极小值的新CCD时间
Q4 Physics and Astronomy Pub Date : 2017-07-03 DOI: 10.22444/IBVS.6202
Kim Chun-Hwey, Kim Hyun-woo, Park Jang-Ho, Song Mi-Hwa, Jeong Min-Ji, Kim Hye-Young
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引用次数: 2
BN Pegasi - A Semidetached Eclipsing Binary BN飞马座-半分离食双星
Q4 Physics and Astronomy Pub Date : 2017-07-03 DOI: 10.22444/IBVS.6201
R. Nelson
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引用次数: 0
V2197 Cyg - A Semi-Detached Eclipsing Binary? V2197Cyg-一个半分离的食双星?
Q4 Physics and Astronomy Pub Date : 2017-07-03 DOI: 10.22444/IBVS.6203
H. Robert, M. R. Russell
The variability of V2197 Cyg (NSVS 5761314, TYC 3167-1279-1), amongst many oth-ers, was discovered photographically by Margoni & Stagni (1984, hereafter M&S) who gave coordinates, magnitude ranges in B and V , finder charts for all 99 stars, elements (epoch, period), and preliminary light curves for about half the stars (but not for V2176 Cyg, their #58). Andronov et al. (1993) performed U, B, V, R , and I photometry of this and three other M&S stars; they went on in Andronov et al. (1994) to identify the system as an eclipsing variable, also giving the elements (including period = 0.46771 d) and eclipse duration. Skiff (1997) identified the M&S variables with those in the IRAS and GSC catalogues. Hoffman et al. (2008) provided an updated period, quoted 2MASS colours, and classified the system as β Lyrae. Since then, there have been a number of eclipse timings but no light curve analysis. examine difference O
在许多其他恒星中,V2197 Cyg(NSVS 5761314,TYC 3167-1279-1)的可变性是由Margoni和Stagni(1984,以下简称M&S)通过摄影发现的,他们给出了坐标、B和V的星等范围、所有99颗恒星的海图、元素(历元、周期)和大约一半恒星的初步光曲线(但V2176 Cyg,它们的#58)。安德罗诺夫等人(1993)对这颗恒星和其他三颗M&S恒星进行了U、B、V、R和I测光;他们在Andronov等人(1994)中继续将该系统确定为食变量,并给出了元素(包括周期=0.46771天)和食持续时间。Ski efff(1997)将M&S变量与IRAS和GSC目录中的变量进行了识别。Ho ffeman等人(2008)提供了一个更新周期,引用了2MASS的颜色,并将该系统分类为βLyrae。从那时起,已经有了一些日食时间,但没有光照曲线分析。检查差异O
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引用次数: 0
DD CMa: A New Galactic DPV of Extreme Short Period DD CMa:一种新的极短周期星系DPV
Q4 Physics and Astronomy Pub Date : 2017-05-14 DOI: 10.22444/IBVS.6207
R. Mennickent, B. Gürol
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引用次数: 1
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Information Bulletin on Variable Stars
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