First photometric and orbital period investigations of the total-eclipse contact binary V0339 Com

New Astronomy ◽  
2021 ◽  
pp. 101695
Author(s):  
Yun-Xia Yu ◽  
Qing Li ◽  
Hui-Ping Huang ◽  
Ke Hu ◽  
Fu-Yuan Xiang
Keyword(s):  
Orbital Period ◽  
Total Eclipse ◽  
Contact Binary

scholarly journals RW Doradus: A solar-type shallow contact binary with a new orbital period investigation

2019 ◽  
Author(s):  
Thawicharat Sarotsakulchai ◽  
Sheng-Bang Qian ◽  
Boonrucksar Soonthornthum ◽  
Eduardo Fernández Lajús ◽  
Nian-Ping Liu ◽  
...  
Keyword(s):  
Orbital Period ◽  
Contact Binary ◽  
Solar Type

scholarly journals A Bright Spot and a Serendipitous Stellar Flare on the Contact-Binary VW Cep

1983 ◽  
Vol 71 ◽  
pp. 481-483
Author(s):  
K.E. Egge ◽  
B.R. Pettersen
Keyword(s):  
Orbital Period ◽  
Triple System ◽  
Bright Spot ◽  
Stellar Flare ◽  
Flare Event ◽  
Main Contributor ◽  
The Third ◽  
Contact Binary ◽  
Photoelectric Observations ◽  
Large Flare

Almost twenty years ago a large flare event was observed on the prototype contact binary W UMa by Kuhi (1964). Similar events have been reported on 44 i Boo (Eggen 1948) and U Peg (Huruhata 1952) . In this paper we present photoelectric observations at three wavelengths of a flare on VW Cep. This is the first event of this kind to be reported for this star. VW Cep is a triple system. The main contributor to the visual flux is the eclipsing binary, consisting of a Kl primary and a G6 secondary (Kopal 1978), classified to be in contact. The orbital period is 6h 41m. Seven per cent of the total flux in the visual filter is due to the third component, a late K type dwarf at a distance of 12 AU from the eclipsing system (Hershey 1975).

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.

scholarly journals Orbital Period Changes for the Weak-Contact Binary TY Bootis

2007 ◽  
Vol 134 (1) ◽  
pp. 179-184 ◽  
Author(s):  
Y.-G. Yang ◽  
J.-M. Dai ◽  
X.-G. Yin ◽  
F.-Y. Xiang
Keyword(s):  
Orbital Period ◽  
Contact Binary ◽  
Weak Contact

Orbital period changes and photometric study of contact binary system AK Her

New Astronomy ◽  
2010 ◽  
Vol 15 (4) ◽  
pp. 339-342 ◽  
Author(s):  
A. Samadi ◽  
D.M.Z. Jassur ◽  
S. Nassiri ◽  
G. Gozaliasl ◽  
M.H. Kermani ◽  
...  
Keyword(s):  
Binary System ◽  
Orbital Period ◽  
Photometric Study ◽  
Contact Binary

Physical Parameters for a Contact Binary AY Aquarius

2014 ◽  
Vol 979 ◽  
pp. 20-22 ◽  
Author(s):  
Wiraporn Maithong ◽  
Chatchai Kruea-In ◽  
Somsawat Rattanasoon
Keyword(s):  
Binary System ◽  
Physical Properties ◽  
Orbital Period ◽  
Physical Parameters ◽  
Contact Binary

The physical parameters study of contact binary system AY Aquarius, the observations were done in 12th September 2011 at The Cerro Tololo Inter-American Observatory (CTIO), Chile. The Prompt4 0.4 - meter Ritchey-Chretien reflecting telescope and CCD Apogee Alta 10241024 pixels with standard visual and red filters of UBV were used. The orbital period of the contact binary system is about 0.28199 days. The photometry was analyzed by MaxIm program and used Wilson-Devinney technique to calculate the physical properties.

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