KIC 5197256: an eclipsing binary containing a δ Scuti variable star

2021 ◽  
Vol 21 (9) ◽  
pp. 224
Author(s):  
Cheng-Long Lv ◽  
Ali Esamdin ◽  
Jun-Hui Liu ◽  
Xiang-Yun Zeng ◽  
Tao-Zhi Yang
Keyword(s):  
Variable Star ◽  
Eclipsing Binary

scholarly journals The dynamical mass of a classical Cepheid variable star in an eclipsing binary system

Nature ◽  
2010 ◽  
Vol 468 (7323) ◽  
pp. 542-544 ◽  
Author(s):  
G. Pietrzyński ◽  
I. B. Thompson ◽  
W. Gieren ◽  
D. Graczyk ◽  
G. Bono ◽  
...  
Keyword(s):  
Binary System ◽  
Variable Star ◽  
Dynamical Mass ◽  
Eclipsing Binary ◽  
Classical Cepheid

scholarly journals A New Binary Star System of EW Type in Draco: GSC 03905-01870

2018 ◽  
Author(s):  
Salvador Barquin
Keyword(s):  
Light Curve ◽  
Binary Stars ◽  
Variable Star ◽  
Binary Star ◽  
Type I ◽  
Star System ◽  
Primary Minimum ◽  
Eclipsing Binary ◽  
Eclipsing Binary Stars ◽  
Binary Star System

Discovery of a new binary star system (GSC 03905-01870 = USNO-B1.0 1431-0327922 = UCAC4 716-059522) in the Draco constellation is presented. It was discovered during a search for previously unreported eclipsing binary stars through the ASAS-SN database. The shape of the light curve and its characteristics (period of 0.428988±0.000001 d, amplitude of 0.34±0.02 V Mag, primary minimum epoch HJD 2457994.2756±0.0002) indicates that the new variable star is an eclipsing binary of W Ursae Majoris type. I registered this variable star in The International Variable Star Index (VSX), its AAVSO UID is 000-BMP-891.

The MACHO Project LMC Variable Star Inventory.V.Classification and Orbits of 611 Eclipsing Binary Stars

1997 ◽  
Vol 114 ◽  
pp. 326 ◽  
Author(s):  
C. Alcock ◽  
R. A. Allsman ◽  
D. Alves ◽  
T. S. Axelrod ◽  
A. C. Becker ◽  
...  
Keyword(s):  
Binary Stars ◽  
Variable Star ◽  
Eclipsing Binary ◽  
Eclipsing Binary Stars

scholarly journals Symbiotic Eclipsing Binary Star CI CYG. The Cold Component Variability

1988 ◽  
Vol 103 ◽  
pp. 197-197
Author(s):  
T.S. Belyakina
Keyword(s):  
Binary System ◽  
Variable Star ◽  
Binary Star ◽  
Time Interval ◽  
Temperature Variations ◽  
Eclipsing Binary ◽  
Cold Component ◽  
Red Giant ◽  
Eclipsing Binary Star

AbstractIt has been shown that the cold component of CI Cyg eclipsing binary system is a variable star. The amplitude of its light variations is close to with the time interval of 40–60 days.This star being the red giant M4 can be attributed as SR type variability. The light variations is caused by its temperature variations.

scholarly journals Analysis of the Open Cluster NGC 2281

Galaxies ◽  
2021 ◽  
Vol 9 (1) ◽  
pp. 7
Author(s):  
Dirk Terrell ◽  
John Gross ◽  
Walter R. Cooney
Keyword(s):  
Variable Star ◽  
American Association ◽  
Open Cluster ◽  
Standard System ◽  
Proper Motions ◽  
Eclipsing Binary ◽  
Photometric Observations ◽  
Sky Survey ◽  
Gaia Dr2

BV observations of an approximately 68′×48′ field centered on the open cluster NGC 2281 and covering more than 400 nights from 2013 to 2018 are presented. The photometric observations were transformed to the standard system using standards from the American Association of Variable Star Observers Photometric All-sky Survey (APASS) DR10 and analyzed with Gaia DR2 parallaxes and proper motions to determine the distance, age, and metallicity of the cluster. The discovery of an eclipsing binary in the field is discussed.

The Variable Star S Doradus as an Eclipsing Binary.

1943 ◽  
Vol 97 ◽  
pp. 166 ◽  
Author(s):  
Sergei Gaposchkin
Keyword(s):  
Variable Star ◽  
Eclipsing Binary

scholarly journals A Photoelectric Investigation of the Eclipsing Binary V 78 in Omega Centauri (NGC 5139)

1971 ◽  
Vol 15 ◽  
pp. 235-237
Author(s):  
Edward H. Geyer
Keyword(s):  
Globular Cluster ◽  
Globular Clusters ◽  
Variable Star ◽  
Eclipsing Binaries ◽  
Stellar Systems ◽  
Light Elements ◽  
Eclipsing Binary ◽  
Evolved Stars ◽  
Photographic Photometry ◽  
Highly Evolved

The existence of eclipsing binaries, though extremely rare, in stellar systems like globular clusters, should attract the observers, because one could obtain fundamental data on highly evolved stars. The variable star V 78 in the globular cluster NGC 5139, which was found by BAILEY (1901), is one of these rare cases. MARTIN (1938) derived the period P = 1ḍ168118, and showed by means of an extensive photographic photometry that it is an Algol type eclipsing binary. Recently SISTERO et al. (1968, 1969) rediscussed the observations of MARTIN, and with additional measurements derived the following light elements:

On the Inhomogeneity of Chemical Composition over the Surface of 21 Per

1976 ◽  
Vol 32 ◽  
pp. 343-349
Author(s):  
Yu.V. Glagolevsky ◽  
K.I. Kozlova ◽  
V.S. Lebedev ◽  
N.S. Polosukhina
Keyword(s):  
Chemical Composition ◽  
Spectral Line ◽  
Variable Star ◽  
Radial Velocities ◽  
Crimean Astrophysical Observatory ◽  
Line Intensities ◽  
Magnetic Variable

SummaryThe magnetic variable star 21 Per has been studied from 4 and 8 Å/mm spectra obtained with the 2.6 - meter reflector of the Crimean Astrophysical Observatory. Spectral line intensities (Wλ) and radial velocities (Vr) have been measured.

The Eclipsing Binary WX Eridani

1979 ◽  
Vol 46 ◽  
pp. 385
Author(s):  
M.B.K. Sarma ◽  
K.D. Abhankar
Keyword(s):  
Light Curve ◽  
Spectral Type ◽  
Orbital Period ◽  
Primary Component ◽  
Light Curves ◽  
Absorption Feature ◽  
Primary Star ◽  
Eclipsing Binary ◽  
The Times ◽  
Phase Angles

AbstractThe Algol-type eclipsing binary WX Eridani was observed on 21 nights on the 48-inch telescope of the Japal-Rangapur Observatory during 1973-75 in B and V colours. An improved period of P = 0.82327038 days was obtained from the analysis of the times of five primary minima. An absorption feature between phase angles 50-80, 100-130, 230-260 and 280-310 was present in the light curves. The analysis of the light curves indicated the eclipses to be grazing with primary to be transit and secondary, an occultation. Elements derived from the solution of the light curve using Russel-Merrill method are given. From comparison of the fractional radii with Roche lobes, it is concluded that none of the components have filled their respective lobes but the primary star seems to be evolving. The spectral type of the primary component was estimated to be F3 and is found to be pulsating with two periods equal to one-fifth and one-sixth of the orbital period.

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