Eclipsing Binaries in the OGLE Variable Star Catalogs. V. Long-Period EB-Type Light Curve Systems in the Small Magellanic Cloud and the PLC-β Relation

2001 ◽  
Vol 121 (1) ◽  
pp. 254-266 ◽  
Author(s):  
Slavek M. Rucinski ◽  
Carla Maceroni
Keyword(s):  
Light Curve ◽  
Variable Star ◽  
Magellanic Cloud ◽  
Eclipsing Binaries ◽  
Small Magellanic Cloud ◽  
Long Period ◽  
Star Catalogs

scholarly journals Decoding of the Light Changes in Wolf-Rayet Eclipsing Binaries: An Application to HD 5980 in the Small Magellanic Cloud

1991 ◽  
Vol 143 ◽  
pp. 229-236
Author(s):  
J. Breysacher ◽  
C. Perrier
Keyword(s):  
Light Curve ◽  
Magellanic Cloud ◽  
Curve Analysis ◽  
Eclipsing Binaries ◽  
Small Magellanic Cloud ◽  
Light Curve Analysis ◽  
Eclipsing Binary ◽  
Preliminary Results ◽  
Limb Darkening

A method of light curve analysis is described which allows the study of an eccentric partially-eclipsing system containing one component possessing an extended atmosphere. The effects of transparency as well as limb-darkening are taken into account. Preliminary results obtained for the Wolf-Rayet eclipsing binary HD 5980 in the SMC are presented.

scholarly journals The distance to the Small Magellanic Cloud from eclipsing binaries

2012 ◽  
Vol 8 (S289) ◽  
pp. 222-225 ◽  
Author(s):  
Dariusz Graczyk ◽  
Grzegorz Pietrzyński ◽  
Bogumił Pilecki ◽  
Ian B. Thompson ◽  
Wolfgang Gieren ◽  
...  
Keyword(s):  
Binary System ◽  
Systematic Error ◽  
Orbital Period ◽  
Surface Brightness ◽  
Magellanic Cloud ◽  
Eclipsing Binaries ◽  
Distance Modulus ◽  
Small Magellanic Cloud ◽  
Eclipsing Binary ◽  
Long Period

AbstractA preliminary distance etimate to SMC 108.1.14904, a long-period eclipsing binary in the Small Magellanic Cloud, is presented. The binary system contains two bright, non-active G-type giants. Its orbital period is 185 days and the orbit is circular. Using surface brightness calibration, we obtain a distance modulus to the system of (m-M)= 19.02 ± 0.04 (statistical) ± 0.05 (systematic) mag, where the systematic error is dominated by uncertainties in the surface brightness calibration. This is a second eclipsing binary in the SMC analysed by our team.

The MACHO Project Large Magellanic Cloud Variable Star Inventory. XII. Three Cepheid Variables in Eclipsing Binaries

2002 ◽  
Vol 573 (1) ◽  
pp. 338-350 ◽  
Author(s):  
C. Alcock ◽  
R. A. Allsman ◽  
D. R. Alves ◽  
A. C. Becker ◽  
D. P. Bennett ◽  
...  
Keyword(s):  
Variable Star ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Eclipsing Binaries ◽  
Cepheid Variables

scholarly journals Long period variables detected by ISO in the Small Magellanic Cloud

2003 ◽  
Vol 406 (1) ◽  
pp. 51-63 ◽  
Author(s):  
M.-R. L. Cioni ◽  
J. A. D. L. Blommaert ◽  
M. A. T. Groenewegen ◽  
H. J. Habing ◽  
J. Hron ◽  
...  
Keyword(s):  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
Long Period ◽  
Long Period Variables

scholarly journals THE ARAUCARIA PROJECT. THE DISTANCE TO THE SMALL MAGELLANIC CLOUD FROM LATE-TYPE ECLIPSING BINARIES

2013 ◽  
Vol 780 (1) ◽  
pp. 59 ◽  
Author(s):  
Dariusz Graczyk ◽  
Grzegorz Pietrzyński ◽  
Ian B. Thompson ◽  
Wolfgang Gieren ◽  
Bogumił Pilecki ◽  
...  
Keyword(s):  
Magellanic Cloud ◽  
Eclipsing Binaries ◽  
Small Magellanic Cloud ◽  
Late Type

scholarly journals Blue and yellow long-period variables in the direction of the Small Magellanic Cloud

2006 ◽  
Vol 457 (3) ◽  
pp. 949-961 ◽  
Author(s):  
R. E. Mennickent ◽  
L. Cidale ◽  
G. Pietrzyński ◽  
W. Gieren ◽  
B. Sabogal
Keyword(s):  
Magellanic Cloud ◽  
Small Magellanic Cloud ◽  
Long Period ◽  
Long Period Variables
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