[PDF] Top 20 COMMISSIONS 27 AND 42 OF THE IA U INF ORMA TION BULLETIN ON VARIABLE ST ARS
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COMMISSIONS 27 AND 42 OF THE IA U INF ORMA TION BULLETIN ON VARIABLE ST ARS
... Magnitudes were determined in a stereomicroscope using comparison stars taken from the Guide Star Catalogue GSC, Lasker et al.. The yellow-light magnitudes `mv' shown in Table 2 are thus[r] ... See full document
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COMMISSIONS 27 AND 42 OF THE IA U INF ORMA TION BULLETIN ON VARIABLE ST ARS
... Due to the limitation of the IBVS format we present in these gures the amplitude spectra and spectral windows for the di erential photometry of the Bootis and one comparison star up to [r] ... See full document
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COMMISSIONS 27 AND 42 OF THE IA U INF ORMA TION BULLETIN ON VARIABLE ST ARS
... LD 229 21 36 50.8 +54 40 58 A 21352+5427 LD 230 21 40 06.2 +59 35 43 A 21386+5922 LD 231 21 44 03.8 +66 39 12 A 21429+6625 LD 232 21 48 25.2 +58 00 53 A 21468+5747 LD 233 21 48 17.9 +62 38 07 A 21469+6224 LD 234 21 50 ... See full document
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COMMISSIONS 27 AND 42 OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS
... be variable by the Japanese amateur astronomer Akira Takao (Kita-kyushu, Japan) in the year 2001 with an average (unfiltered) ∼ 13 mag (Kazarovets et ...ERSO 27, with a spectral type SX/6e: no special ... See full document
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COMMISSIONS 27 AND 42 OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS
... In this 81st compilation of BAV results, photoelectric observations obtained mostly in the years 2014 ans 2015 are presented on 512 variable stars giving 838 minima on eclipsing binaries and maxima on pulsating ... See full document
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COMMISSIONS 27 AND 42 OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS
... of Variable Stars (Kazarovets et ...1952 variable stars recently named in the system of designa- tions of the GCVS (General Catalogue of Variable Stars; Samus et ... See full document
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COMMISSIONS 27 AND 42 OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS
... Perhaps the most interesting feature of Figure 2 is the behavior of Hα emission outside of eclipse. Large fluctuations in EW occurred continuously over about 15 years. A possible explanation might be a variable ... See full document
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COMMISSIONS 27 AND 42 OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS
... Acknowledgement: MS acknowledges the support of the postdoctoral fellowship pro- gramme of the Hungarian Academy of Sciences at the Konkoly Observatory as a host insti- tution. This research made use of the International ... See full document
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COMMISSIONS 27 AND 42 OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS
... Method of data reduction: All observations were reduced and photometry was performed using C-Munipack package http://c-munipack.sourceforge.net/ Method of minimum determination: The mini[r] ... See full document
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COMMISSIONS 27 AND 42 OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS
... The comparison of this mean curve with the present data reveals that the object was in the active state during the autumn observations, see Fig. 1. A flare observed on JD 2455835 supports such an idea. It is interesting ... See full document
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COMMISSIONS 27 AND 42 OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS
... Like in the case of NL 80, we separate the catalogue of newly designated variables (to be presented at the GCVS web site) from the Name-List proper. Table 1 of the current Name-List contains the new GCVS name, equatorial ... See full document
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COMMISSIONS 27 AND 42 OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS
... An account of the multiple star η Mus (HD 114911, HIP 64661, HR 4993) was given by Budding et al. (2013). The light is dominated by the young close binary (V ∼ 4.8- 4.9, B − V ≈ − 0.08, U − B ≈ − 0.34), which is a ... See full document
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COMMISSIONS 27 AND 42 OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS
... Upper right Period analysis of the long-term removed data in the lower left panel.. Lower right Phase diagram of the 509 d period..[r] ... See full document
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COMMISSIONS 27 AND 42 OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS
... Analysis of the rotation maxima The rotation modulation gives rotation maxima trot Figure 1 shows a number of them.. Because of the ambiguities in the cycle counting, there are 4 differe[r] ... See full document
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COMMISSIONS 27 AND 42 OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS
... The separation of the components, necessary to absolutely calibrate masses and sizes, was approximately obtained iteratively adjusting it up to obtain a bolometric magnitude consistent w[r] ... See full document
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COMMISSIONS 27 AND 42 OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS
... Part I of the 80th Name-List of Variable Stars (Kazarovets et al., 2011b) contained information on 2036 stars recently named in the system of the General Catalogue of Variable Stars (GCVS; Samus et al. ... See full document
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COMMISSIONS 27 AND 42 OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS
... The residuals of the observations and of this modelling the F t function, see below were searched for signals at FB1 and FB2 , in the low frequency end of their Fourier spectrum, with ne[r] ... See full document
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OF THE IA INF ORMA TION BULLETIN ON ARIABLE ST ARS
... Table 5 lists oordinates and identi ations for the 107 variable stars found in Table I of the dis overy paper, followed by the 16 variable stars previously dis overed by Luyten, from Hoe[r] ... See full document
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OF THE IA INF ORMA TION BULLETIN ON ARIABLE ST ARS
... Payne-Gapos hkin and Sergei Gapos hkin initiated the task of studying the variable stars in the Magellani Clouds, by analysing the photographi material olle ted on these small galaxies b[r] ... See full document
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COMMISSIONS 27 AND 42 OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS
... discovering variable stars, but unfil- tered or single-filter observations are ineffective at distinguishing different types of variable stars whose light curve shapes are very ...informa- tion, ... See full document
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