scholarly journals Photometry, light curve solution and period study of contact binary BX And

2021 ◽  
pp. 29-36
Author(s):  
M. Partovi ◽  
A. Abedi ◽  
K.Y. Roobiat
Keyword(s):  
Binary Star ◽  
Mass Transfer Rate ◽  
Quadratic Function ◽  
Contact Binary ◽  
The University ◽  
Astronomical Image Processing ◽  
Curve Solution ◽  
Light Curve Solution ◽  
Radial Velocity Data ◽  
Periodic Changes

The photometry of the binary star BX And (HIP 10027) is performed during several nights in October and November 2019, and October 2020 using B, V, and R Johnson-Cousins filters in Dr. Mojtahedi Observatory of the University of Birjand. Astronomical image processing and data reduction are performed by the IRIS software and light curves are obtained. These curves, along with the radial velocity data of the binary star, are analyzed by the Phoebe program to determine the physical and geometric parameters of the system. The evolutionary state of this system is investigated using the Hertzsprung-Russell (H-R) and density vs color index diagrams. The O-C curve is plotted using the eclipse times obtained in this study and those reported in the literature. By fitting a quadratic function to this curve, a new linear ephemeris is obtained for the system, and the mass transfer rate between the components of the system is determined. A periodic behavior is observed in the residuals, after subtracting the quadratic function from the O-C curve. These periodic changes are attributed to the presence of a third component in the system. The parameters of the third component are determined by fitting the light-time function to the residuals curve.

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.

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 The First Light Curve Solution of GW Leo and Refined Ephemeris of Two Contact Binary Systems

2021 ◽  
Vol 65 (7) ◽  
pp. 543-551
Author(s):  
A. Poro ◽  
A. Halavati ◽  
E. Lashgari ◽  
F. Davoudi ◽  
A. Gardi ◽  
...  
Keyword(s):  
Light Curve ◽  
Binary Systems ◽  
Contact Binary ◽  
Curve Solution ◽  
Light Curve Solution

scholarly journals Infrared spectroscopy of the merger candidate KIC 9832227

2018 ◽  
Vol 615 ◽  
pp. A120 ◽  
Author(s):  
Ya. V. Pavlenko ◽  
A. Evans ◽  
D. P. K. Banerjee ◽  
J. Southworth ◽  
M. Shahbandeh ◽  
...  
Keyword(s):  
Infrared Spectroscopy ◽  
Near Infrared ◽  
Binary Star ◽  
Circumstellar Envelope ◽  
Stellar Rotation ◽  
Coronal Activity ◽  
Orbital Phase ◽  
Solar Metallicity ◽  
Contact Binary ◽  
The Individual

Context. It has been predicted that the object KIC 9832227 – a contact binary star – will undergo a merger in 2022.2 ± 0.7. We describe the near-infrared (NIR) spectrum of this object as an impetus to obtain pre-merger data. Aims. We aim to characterise (i) the nature of the individual components of the binary and (ii) the likely circumbinary environment, so that the merger – if and when it occurs – can be interpreted in an informed manner. Methods. We use infrared (IR) spectroscopy in the wavelength range 0.7–2.5 μm, to which we fit model atmospheres to represent the individual stars. We use the binary ephemeris to determine the orbital phase at the time of observation. Results. We find that the IR spectrum is best fitted by a single component with effective temperature 5920 K, log[g] = 4.1, and solar metallicity, consistent with the fact that the system was observed at conjunction. Conclusions. The strength of the IR H lines is consistent with a high value of logg, and the strength of the Ca II triplet indicates the presence of a chromosphere, as might be expected from rapid stellar rotation. The He I absorption we observe likely arises in He excited by coronal activity in a circumstellar envelope, suggesting that the weakness of the Ca II triplet is also likely chromospheric in origin.

scholarly journals Origin of the orbital period change in contact binary stars

2019 ◽  
Vol 28 (06) ◽  
pp. 1950044 ◽  
Author(s):  
V. V. Sargsyan ◽  
H. Lenske ◽  
G. G. Adamian ◽  
N. V. Antonenko
Keyword(s):  
Orbital Period ◽  
Binary Stars ◽  
Binary Systems ◽  
Binary Star ◽  
Period Change ◽  
Mass Asymmetry ◽  
Contact Binary Stars ◽  
Contact Binary ◽  
Energy Formula ◽  
Orbital Periods

The evolution of contact binary star systems in mass asymmetry (transfer) coordinate is considered. The orbital period changes are explained by an evolution in mass asymmetry towards the symmetry (symmetrization of binary system). It is predicted that decreasing and increasing orbital periods are related, respectively, with the nonoverlapping and overlapping stage of the binary star during its symmetrization. A huge amount of energy [Formula: see text][Formula: see text]J is converted from the potential energy into internal energy of the stars during the symmetrization. As shown, the merger of stars in the binary systems, including KIC 9832227, is energetically an unfavorable process. The sensitivity of the calculated results to the values of total mass and orbital angular momentum is analyzed.

Absolute parameters of the newly-identified contact binary star IS Canis Major

New Astronomy ◽  
2010 ◽  
Vol 15 (2) ◽  
pp. 247-253 ◽  
Author(s):  
B. Özkardeş ◽  
A. Erdem
Keyword(s):  
Binary Star ◽  
Contact Binary ◽  
Absolute Parameters

The near-contact binary star RZ Dra revisited

New Astronomy ◽  
2011 ◽  
Vol 16 (1) ◽  
pp. 6-11 ◽  
Author(s):  
A. Erdem ◽  
S. Zola ◽  
M. Winiarski
Keyword(s):  
Binary Star ◽  
Contact Binary

A CCD PHOTOMETRIC STUDY OF THE CONTACT BINARY STAR GSC 03526-01995

2012 ◽  
Vol 144 (6) ◽  
pp. 178 ◽  
Author(s):  
W.-P. Liao ◽  
S.-B. Qian ◽  
N.-P. Liu
Keyword(s):  
Binary Star ◽  
Photometric Study ◽  
Contact Binary

scholarly journals Photometric study of the over-contact binary star GSC 3822-1056

2003 ◽  
Vol 403 (2) ◽  
pp. 637-643 ◽  
Author(s):  
Sz. Csizmadia ◽  
I. B. Bíró ◽  
T. Borkovits
Keyword(s):  
Binary Star ◽  
Photometric Study ◽  
Contact Binary
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