| ZHANG, B., Shengbang QIAN, Miloslav ZEJDA, Liying ZHU a Nianping LIU. 1SWASP J200503.05-343726.5: A high mass ratio eclipsing binary near the period limit. New Astronomy. AMSTERDAM: Elsevier Science, 2017, roč. 54, July, s. 52-55. ISSN 1384-1076. Dostupné z: https://dx.doi.org/10.1016/j.newast.2017.01.007. |
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@article{1401973,
author = {Zhang, B. and Qian, Shengbang and Zejda, Miloslav and Zhu, Liying and Liu, Nianping},
article_location = {AMSTERDAM},
article_number = {July},
doi = {http://dx.doi.org/10.1016/j.newast.2017.01.007},
keywords = {Binary; Eclipsing binary; Short-period limit; Light curves},
language = {eng},
issn = {1384-1076},
journal = {New Astronomy},
title = {1SWASP J200503.05-343726.5: A high mass ratio eclipsing binary near the period limit},
volume = {54},
year = {2017}
}
TY - JOUR
ID - 1401973
AU - Zhang, B. - Qian, Shengbang - Zejda, Miloslav - Zhu, Liying - Liu, Nianping
PY - 2017
TI - 1SWASP J200503.05-343726.5: A high mass ratio eclipsing binary near the period limit
JF - New Astronomy
VL - 54
IS - July
SP - 52-55
EP - 52-55
PB - Elsevier Science
SN - 13841076
KW - Binary
KW - Eclipsing binary
KW - Short-period limit
KW - Light curves
N2 - First CCD photometric light curves of the eclipsing binary system 1SWASP J200503.05-343726.5 are presented. Our complete light curves in V, R and I bands using the Bessell filter show an out-of-eclipsing distortion, which means that the components of the system may be active. The preliminary photometric solutions with a cool star-spot are derived by using the 2013 version of the Wilson-Devinney (W-D) code. The photometric solutions suggest that 1SWASP J200503.05-343726.5 is a shallow-contact eclipsing binary(f = 9.0%) with a mass ratio of q= 1.0705, which is very high for late-type binary systems near the period limit. The primary component is about 230 K hotter than the secondary component. Based on our new CCD eclipse times, the orbital period change was analyzed. According to 0 C diagram, the orbital period of the 1SWASP 1200503.05-343726.5 shows an increase at a rate of <(P)over dot> = +5.43 x 10(-8) days year(-1). The period increase may be caused by mass transfer from the less massive component to the more massive one. This shallow-contact system may be formed from a detached short-period binary via orbital shrinkage because of dynamical interactions with a third component or by magnetic braking. (C) 2017 Elsevier B.V. All rights reserved.
ER -
ZHANG, B., Shengbang QIAN, Miloslav ZEJDA, Liying ZHU a Nianping LIU. 1SWASP J200503.05-343726.5: A high mass ratio eclipsing binary near the period limit. \textit{New Astronomy}. AMSTERDAM: Elsevier Science, 2017, roč.~54, July, s.~52-55. ISSN~1384-1076. Dostupné z: https://dx.doi.org/10.1016/j.newast.2017.01.007.
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