scholarly journals Apsidal motion and a light curve solution for eighteen SMC eccentric eclipsing binaries

2014 ◽  
Vol 572 ◽  
pp. A71 ◽  
Author(s):  
P. Zasche ◽  
M. Wolf ◽  
J. Vraštil ◽  
J. Liška ◽  
M. Skarka ◽  
...  
Keyword(s):  
Light Curve ◽  
Eclipsing Binaries ◽  
Apsidal Motion ◽  
Curve Solution ◽  
Light Curve Solution

scholarly journals APSIDAL MOTION AND A LIGHT CURVE SOLUTION FOR 13 LMC ECCENTRIC ECLIPSING BINARIES

2015 ◽  
Vol 150 (6) ◽  
pp. 183 ◽  
Author(s):  
P. Zasche ◽  
M. Wolf ◽  
J. Vraštil ◽  
L. Pilarčík
Keyword(s):  
Light Curve ◽  
Eclipsing Binaries ◽  
Apsidal Motion ◽  
Curve Solution ◽  
Light Curve Solution

scholarly journals UBVRI Photometric Analysis of the Solar-Type Eclipsing Binary TYC 3034-299-1

2012 ◽  
Vol 2012 ◽  
pp. 1-11
Author(s):  
Ronald G. Samec ◽  
Adam Jaso ◽  
Jesse White ◽  
Danny R. Faulkner ◽  
Nicholas Blum ◽  
...  
Keyword(s):  
Light Curve ◽  
Massive Star ◽  
Light Curves ◽  
Dark Spot ◽  
Mass Ratio ◽  
Photometric Analysis ◽  
Contact Binary ◽  
Solar Type ◽  
Curve Solution ◽  
Light Curve Solution

TYC 3034-0299-1 (CVn) is a magnetically active, contact binary, ROTSE variable. UBVRcIc light curves are presented along with a period study and a simultaneous UBVRI light curve solution. Our light curves show eclipse amplitudes of 0.72 and 0.62 mags (V) in the primary and secondary eclipses. Modeled results include a dark spot region, found at longitude 51°, a 24% Roche lobe fill-out, and a mass ratio of 0.48. A total eclipse is found to occur in the secondary eclipse making TYC 3034-0299-1 a W-type (less massive star is hotter) W UMa variable.

scholarly journals BVRcIc Observations and Analysis of the Near-Contact Solar Type Eclipsing Binary, V530 Andromedae

2013 ◽  
Vol 2013 ◽  
pp. 1-8
Author(s):  
Ronald G. Samec ◽  
Daniel Flaaten ◽  
James Kring ◽  
Danny R. Faulkner
Keyword(s):  
Light Curve ◽  
Undergraduate Research ◽  
Initial Period ◽  
Light Curves ◽  
Eclipsing Binary ◽  
Massive Component ◽  
Solar Type ◽  
First Time ◽  
Curve Solution ◽  
Light Curve Solution

We present the first precision UBVRcIc light curves, an initial period study, and a simultaneous light curve solution for the near-contact solar type eclipsing binary V530 And. Our observations were taken with the 0.81 m Lowell reflector on 27 and 29 September, 2011, with time being granted from the National Undergraduate Research Observatory (NURO). Our Wilson Devinney Program solution yields a semidetached, V1010 Oph configuration: the more massive component is filling its Roche lobe. The system is apparently approaching contact for the first time. It is not a classic Algol.

Light curve solution and orbital period analysis of the contact binary V842 Herculis

2005 ◽  
Vol 326 (8) ◽  
pp. 746-753 ◽  
Author(s):  
S. O. Selam ◽  
B. Albayrak ◽  
H. V. Şenavci ◽  
O. Aksu
Keyword(s):  
Light Curve ◽  
Orbital Period ◽  
Period Analysis ◽  
Contact Binary ◽  
Curve Solution ◽  
Light Curve Solution

scholarly journals Improved Light Curves of LMC Eclipsing Binaries

2005 ◽  
Vol 13 ◽  
pp. 461-461
Author(s):  
Young Woon Kang ◽  
Kyungsoo Hong ◽  
Woo-Baik Lee ◽  
Ho-Il Kim ◽  
Kyu-Dong Oh
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Eclipsing Binaries ◽  
Light Curves ◽  
Dispersion Method ◽  
Direct Observations ◽  
Continuum Energy ◽  
Curve Solution ◽  
Light Curve Solution ◽  
The Continuum

We present accurate BV light curves and continuum energy curves of the EROS eclipsing binaries in the Large Magellanic Cloud to find accurate binary parameters as well as their distances. The observations have been carried out using the 2.1 meter telescope in CASLEO Argentina during Feb. 1-10, 2003. We have concentrated CCD direct observations upon EROS field 1 and 2 to improve the accuracy of light curves of eclipsing binaries in the fields. The spectroscopic observations have been also carried out using the simple dispersion method to get continuum energy curves between wavelengths of 4000-8000 Å for several EROS eclipsing binaries. At first, we determined a combined temperature of both components of each binary system using the continuum. Then, the combined temperature was resolved using the first estimation of the light curve solution. Finally, we determined the photometric solutions of several binaries in the Large Magellanic Cloud.

Light-curve solution and interpretation for CG Cygni

1985 ◽  
Vol 90 ◽  
pp. 761 ◽  
Author(s):  
S. A. Naftilan ◽  
E. F. Milone
Keyword(s):  
Light Curve ◽  
Curve Solution ◽  
Light Curve Solution

scholarly journals Photometry of RZ Ophiuchi - an international collaboration

1986 ◽  
Vol 118 ◽  
pp. 299-300
Author(s):  
L.B.G. Knee ◽  
C. D. Scarfe ◽  
B. W. Baldwin ◽  
S. J. Meatheringham
Keyword(s):  
Mass Transfer ◽  
Light Curve ◽  
International Collaboration ◽  
Late Stage ◽  
Roche Lobe ◽  
Temperature Calibration ◽  
Curve Solution ◽  
Light Curve Solution

UBV observations, plus a few in R and I, were obtained during the 1984 eclipse of RZ Ophiuchi. Bolometric corrections and temperature calibration, applied to the magnitudes and colours of the stars, were used to derive the ratio of the stellar radii, and a light curve solution was obtained with this parameter fixed. Neither component fills its Roche lobe, but the system may be at a late stage of case C mass transfer.

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