Short-Period Light Variation of an Eclipsing Binary System: RZ Cassiopeiae

2001 ◽  
Vol 122 (1) ◽  
pp. 418-424 ◽  
Author(s):  
Osamu Ohshima ◽  
Shin-ya Narusawa ◽  
Hidehiko Akazawa ◽  
Kikuichi Arai ◽  
Mitsugu Fujii ◽  
...  
Keyword(s):  
Binary System ◽  
Light Variation ◽  
Eclipsing Binary ◽  
Short Period

scholarly journals Variability of the Light Curves of the Close Binary GR Tauri

2002 ◽  
Vol 187 ◽  
pp. 337-338
Author(s):  
A. Yamasaki ◽  
M. Takeda ◽  
T. Yamauchi ◽  
G. Takada ◽  
S. Hattori
Keyword(s):  
Binary System ◽  
The State ◽  
Light Curves ◽  
Close Binary ◽  
Eclipsing Binary ◽  
Short Period ◽  
Contact Binary

AbstractVariability of the light curves of the short-period eclipsing binary system GR Tau (, almost-contact binary) is studied. It is found that GR Tau experienced both the state which is characterized by asymmetric light curves and the state characterized by symmetrical light curves.

The first CCD photometric analysis and modeling for short period eclipsing binary system 1SWASPJ210423.7+073140.4.

New Astronomy ◽  
2016 ◽  
Vol 47 ◽  
pp. 24-28
Author(s):  
M.S. Saad ◽  
M.S. Darwish ◽  
M.A. Nasser ◽  
M.A. Hamdy ◽  
M.M. Beheary ◽  
...  
Keyword(s):  
Binary System ◽  
Photometric Analysis ◽  
Eclipsing Binary ◽  
Short Period

scholarly journals LB 3459, a short-period eclipsing binary system containing two O-type subdwarfs

1978 ◽  
Vol 183 (3) ◽  
pp. 523-531 ◽  
Author(s):  
D. Kilkenny ◽  
R. W. Hilditch ◽  
J. E. Penfold
Keyword(s):  
Binary System ◽  
Eclipsing Binary ◽  
Short Period

scholarly journals WZ Sge: Recent Observations Leading to a Model for Superhump Phenomena

1979 ◽  
Vol 53 ◽  
pp. 458-458
Author(s):  
R. L. Gilliland ◽  
E. Kemper
Keyword(s):  
Binary System ◽  
Absorption Line ◽  
Radial Velocities ◽  
Schematic Model ◽  
Dwarf Novae ◽  
Eclipsing Binary ◽  
Gaseous Disk ◽  
Short Period ◽  
Hα Emission ◽  
Recurrent Nova

AbstractThe short period eclipsing binary system and recurrent nova WZ Sge (1913, 1946, 1978) was observed spectroscopically during its renewed, December 1978 outburst. Absorption line radial velocities and Hα emission profiles suggest a clrcumblnary gaseous disk. A schematic model is presented to explain both the observed radial velocities and the photometric properties of WZ Sge during outburst. The model also accounts for ‘superhump’ phenomena in SU UMa type dwarf novae.

1SWASP J034439.97+030425.5: a short-period eclipsing binary system with a close-in stellar companion

2020 ◽  
Vol 20 (4) ◽  
pp. 047
Author(s):  
Bin Zhang ◽  
Sheng-Bang Qian ◽  
Jing-Jing Wang ◽  
Qi-Jun Zhi ◽  
Ai-Jun Dong ◽  
...  
Keyword(s):  
Binary System ◽  
Eclipsing Binary ◽  
Short Period

scholarly journals The eclipsing binary IU Per and its intrinsic oscillations

2008 ◽  
Vol 4 (S252) ◽  
pp. 429-430
Author(s):  
X. B. Zhang
Keyword(s):  
Time Series ◽  
Binary System ◽  
Fourier Analysis ◽  
Primary Component ◽  
Eclipsing Binary ◽  
Mode Identification ◽  
Short Period ◽  
Photometric Solution

AbstractThe results of a long-term time-series photometry of the short-period eclipsing binary IU Per are reported. The observation confirms the intrinsic δ Scuti-like pulsation of the star as discovered by previous authors. A photometric solution for the binary system was carried out with the new data. Based on which, the pure oscillation light variations from the mass-accreting primary component were extracted. A Fourier analysis reveals four pulsation modes. Combining with the photometric solution, a preliminary mode identification was given.

scholarly journals X-ray and UV emission of the ultrashort-period, low-mass eclipsing binary system BX Trianguli

2018 ◽  
Vol 619 ◽  
pp. A138
Author(s):  
V. Perdelwitz ◽  
S. Czesla ◽  
J. Robrade ◽  
T. Pribulla ◽  
J. H. M. M. Schmitt
Keyword(s):  
Binary System ◽  
Light Curve ◽  
Binary Systems ◽  
Uv Light ◽  
Close Binary ◽  
Eclipsing Binary ◽  
X Ray ◽  
Uv Emission ◽  
Low Mass ◽  
Orbital Modulation

Context.Close binary systems provide an excellent tool for determining stellar parameters such as radii and masses with a high degree of precision. Due to the high rotational velocities, most of these systems exhibit strong signs of magnetic activity, postulated to be the underlying reason for radius inflation in many of the components. Aims.We extend the sample of low-mass binary systems with well-known X-ray properties. Methods.We analyze data from a singular XMM-Newton pointing of the close, low-mass eclipsing binary system BX Tri. The UV light curve was modeled with the eclipsing binary modeling tool PHOEBE and data acquired with the EPIC cameras was analyzed to search for hints of orbital modulation. Results.We find clear evidence of orbital modulation in the UV light curve and show that PHOEBE is fully capable of modeling data within this wavelength range. Comparison to a theoretical flux prediction based on PHOENIX models shows that the majority of UV emission is of photospheric origin. While the X-ray light curve does exhibit strong variations, the signal-to-noise ratio of the observation is insufficient for a clear detection of signs of orbital modulation. There is evidence of a Neupert-like correlation between UV and X-ray data.

scholarly journals New Data on the Eclipsing Binary V1848 Ori and Improved Orbital and Light Curve Solutions

2020 ◽  
Vol 29 (1) ◽  
pp. 72-80 ◽  
Author(s):  
Fatemeh Davoudi ◽  
Atila Poro ◽  
Fahri Alicavus ◽  
Afshin Halavati ◽  
Saeed Doostmohammadi ◽  
...  
Keyword(s):  
Binary System ◽  
Light Curve ◽  
Mass Function ◽  
Light Curves ◽  
Complete Analysis ◽  
Physical Parameters ◽  
Mass Ratio ◽  
Third Body ◽  
Eclipsing Binary

AbstractNew observations of the eclipsing binary system V1848 Ori were carried out using the V filter resulting in a determination of new times of minima and new ephemeris were obtained. We presented the first complete analysis of the system’s orbital period behavior and analysis of O-C diagram done by the GA and MCMC approaches in OCFit code. The O-C diagram demonstrates a sinusoidal trend in the data; this trend suggests a cyclic change caused by the LITE effect with a period of 10.57 years and an amplitude of 7.182 minutes. It appears that there is a third body with mass function of f (m3) = 0.0058 M⊙ in this binary system. The light curves were analyzed using the Wilson-Devinney code to determine some geometrical and physical parameters of the system. These results show that V1848 Ori is a contact W UMa binary system with the mass ratio of q = 0.76 and a weak fillout factor of 5.8%. The O’Connell effect was not seen in the light curve and there is no need to add spot.

NSVS 11868841: An active detached eclipsing binary system with a substellar object

New Astronomy ◽  
2021 ◽  
pp. 101678
Author(s):  
B. Zhang ◽  
S.-B. Qian ◽  
Q.-J. Zhi ◽  
A.-J. Dong ◽  
L.-Y. Zhu
Keyword(s):  
Binary System ◽  
Eclipsing Binary
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