1SWASP J200503.05-343726.5: A high mass ratio eclipsing binary
near the period limit

J 2017

1SWASP J200503.05-343726.5: A high mass ratio eclipsing binary near the period limit

ZHANG, B., Shengbang QIAN, Miloslav ZEJDA, Liying ZHU, Nianping LIU et. al.

Basic information

Original name

1SWASP J200503.05-343726.5: A high mass ratio eclipsing binary near the period limit

Authors

ZHANG, B. (156 China), Shengbang QIAN (156 China), Miloslav ZEJDA (203 Czech Republic, guarantor, belonging to the institution), Liying ZHU (156 China) and Nianping LIU (156 China)

Edition

New Astronomy, AMSTERDAM, Elsevier Science, 2017, 1384-1076

Other information

Language

English

Type of outcome

Článek v odborném periodiku

Field of Study

10308 Astronomy

Country of publisher

Netherlands

Confidentiality degree

není předmětem státního či obchodního tajemství

Impact factor

Impact factor: 0.920

RIV identification code

RIV/00216224:14310/17:00099154

Organization unit

Faculty of Science

DOI

http://dx.doi.org/10.1016/j.newast.2017.01.007

UT WoS

000397369300007

Keywords in English

Binary; Eclipsing binary; Short-period limit; Light curves

Abstract

V originále

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.

Links

LG15010, research and development project

Name: F. Magellanes: projekt podpory studia hvězd a hvězdných soustav na základě pozorování ze Země a z kosmického prostoru (Acronym: Magellan2015)

Investor: Ministry of Education, Youth and Sports of the CR

Citovat

ZHANG, B., Shengbang QIAN, Miloslav ZEJDA, Liying ZHU and Nianping LIU. 1SWASP J200503.05-343726.5: A high mass ratio eclipsing binary near the period limit. New Astronomy. AMSTERDAM: Elsevier Science, 2017, vol. 54, July, p. 52-55. ISSN 1384-1076. Available from: https://dx.doi.org/10.1016/j.newast.2017.01.007.

@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 and Nianping LIU. 1SWASP J200503.05-343726.5: A high mass ratio eclipsing binary near the period limit. \textit{New Astronomy}. AMSTERDAM: Elsevier Science, 2017, vol.~54, July, p.~52-55. ISSN~1384-1076. Available from: https://dx.doi.org/10.1016/j.newast.2017.01.007.

Detailed Information on Publication Record