First orbital period analysis of the Algol-type eclipsing binary RZ Aurigae

New Astronomy ◽  
2010 ◽  
Vol 15 (4) ◽  
pp. 392-395 ◽  
Author(s):  
Y.-G. Yang ◽  
H.-F. Dai ◽  
X.-G. Yin
Keyword(s):  
Orbital Period ◽  
Period Analysis ◽  
Eclipsing Binary

scholarly journals Light Curve and Orbital Period Analysis of the Eclipsing Binary AT Peg

2011 ◽  
Vol 7 (S282) ◽  
pp. 55-56
Author(s):  
Alexios Liakos ◽  
Panagiotis Niarchos ◽  
Edwin Budding
Keyword(s):  
Light Curve ◽  
Orbital Period ◽  
Time Effect ◽  
Light Curves ◽  
Period Analysis ◽  
Eclipsing Binary ◽  
Secular Changes ◽  
Photometric Observations ◽  
Photometric Elements

AbstractCCD photometric observations of the Algol-type eclipsing binary AT Peg have been obtained. The light curves are analyzed with modern techniques and new geometric and photometric elements are derived. A new orbital period analysis of the system, based on the most reliable timings of minima found in the literature, is presented and apparent period modulations are discussed with respect to the Light-Time effect (LITE) and secular changes in the system. The results of these analyses are compared and interpreted in order to obtain a coherent view of the system's behaviour.

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.

scholarly journals Hi-fi phenomenological description of eclipsing binary light variations as the basis for their period analysis

2013 ◽  
Vol 64 ◽  
pp. 299-302 ◽  
Author(s):  
Z. Mikulášek ◽  
M. Zejda ◽  
M. Chrastina ◽  
S.-B. Qian ◽  
L.-Y. Zhu
Keyword(s):  
Phenomenological Description ◽  
Period Analysis ◽  
Eclipsing Binary

scholarly journals Photometry of the δ Scuti Star DG Leo: Preliminary Results

2004 ◽  
Vol 191 ◽  
pp. 73-74 ◽  
Author(s):  
P. Lampens ◽  
R. Garrido ◽  
L. Parrao ◽  
J.H. Peña ◽  
T. Arentoft ◽  
...  
Keyword(s):  
Orbital Period ◽  
Noise Level ◽  
Amplitude Spectrum ◽  
Slow Variation ◽  
Photoelectric Photometry ◽  
Period Analysis ◽  
Preliminary Results ◽  
Spectroscopic Binary ◽  
Scuti Star ◽  
Triple Star

AbstractNew uvby photoelectric photometry has been acquired for the triple star DG Leo at two different observatories equipped with analogous instrumentation. A preliminary period analysis indicates the presence of at least 3 close δ Scuti frequencies (10-12 c/d, 3-6 mmag) and a slow variation. This slow variation fits quite well with half the orbital period of the spectroscopic binary; the noise level in the amplitude spectrum is only 3–4 mmag (after prewhitening).

scholarly journals Epsilon Aurigae: A Supergiant and a Super Disk

1989 ◽  
Vol 107 ◽  
pp. 336-336
Author(s):  
Sean Carroll ◽  
Edward Guinan ◽  
George McCook ◽  
Robert Donahue
Keyword(s):  
Light Curve ◽  
Orbital Period ◽  
Instability Strip ◽  
Eclipsing Binary ◽  
Characteristic Period ◽  
Photoelectric Observations ◽  
Low Amplitude ◽  
Epsilon Aurigae ◽  
Villanova University

The eclipsing binary Epsilon Aurigae consists of an F0 supergiant and a cool, mysterious eclipsing companion with an orbital period of 27.1 years. The light curve of this system reveals two sources of variability: the eclipses themselves and the intrinsic variation of the supergiant. Multifilter photoelectric observations were made with the 38 cm reflector at the Villanova University Observatory. These data were analyzed along with other sources to reveal the nature of the components of the Epsilon Aurigae system. The system undergoes low-amplitude semi-regular light variations with a characteristic period of 110 days and perhaps a longer period of 500-600 days. The proximity of Epsilon Aur to the Cepheid instability strip on the H-R diagram suggests that the pulsation mechanism for this star may be similar to that of Cepheids.

scholarly journals The multiple system Sk-67°18 in the LMC

1995 ◽  
Vol 163 ◽  
pp. 251-253 ◽  
Author(s):  
V. S. Niemela ◽  
W. Seggewiss ◽  
A. F. J. Moffat
Keyword(s):  
Binary System ◽  
Radial Velocity ◽  
Spectral Type ◽  
Orbital Period ◽  
Large Magellanic Cloud ◽  
Primary Component ◽  
Magellanic Cloud ◽  
Bright Star ◽  
High Mass ◽  
Eclipsing Binary

The bright star Sk—67°18 (Brey 5) in the Large Magellanic Cloud (LMC) contains an eclipsing binary system. Our radial velocity study reveals that the orbital period is almost exactly two days. The spectra also show that the star's primary component is not of spectral type WN, but that the star is rather an Of+O type binary where the primary is probably of type O3f*. Furthermore, Sk—67°18 appears to be a high-mass multiple system.

Period analysis of the eclipsing binary AI Dra

2009 ◽  
Vol 326 (1) ◽  
pp. 119-123 ◽  
Author(s):  
P. Zasche ◽  
R. Uhlář ◽  
P. Svoboda
Keyword(s):  
Period Analysis ◽  
Eclipsing Binary

scholarly journals Orbital Period Change of the Eclipsing Binary System SZ Piscium

2010 ◽  
Vol 62 (3) ◽  
pp. 671-674 ◽  
Author(s):  
Xiao-Liang Wang ◽  
Fu-Yuan Xiang ◽  
Yong-Po Tian ◽  
Xiao-Min Shi
Keyword(s):  
Binary System ◽  
Orbital Period ◽  
Period Change ◽  
Eclipsing Binary
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