The first photometric analysis and period investigation of the K-type W UMa type binary system V0842 Cep
V0842 Cep is a W UMa-type binary star that has been neglected since its discovery. We analysed the VR c I c light curves, obtained by the 1 m telescope at Weihai Observatory of Shandong University, using the Wilson-Devinney code. V0842 Cep was found to be a shallow contact binary system ( f = 8.7%)...
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Published in | Research in astronomy and astrophysics Vol. 21; no. 5; pp. 122 - 202 |
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Main Authors | , , |
Format | Journal Article |
Language | English |
Published |
Beijing
National Astronomical Observatories, CAS and IOP Publishing Ltd
01.06.2021
IOP Publishing Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment,Institute of Space Sciences,Shandong University,Weihai 264209,China%Qilu Institute of Technology,Jinan 250200,China |
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Abstract | V0842 Cep is a W UMa-type binary star that has been neglected since its discovery. We analysed the
VR
c
I
c
light curves, obtained by the 1 m telescope at Weihai Observatory of Shandong University, using the Wilson-Devinney code. V0842 Cep was found to be a shallow contact binary system (
f
= 8.7%) with a mass ratio of 2.281. Because its orbital inclination is greater than 80°, the photometric results are reliable. A period study is included which reveals a continually decreasing orbital period (
d
p
d
t
= 1.50(±0.42)×10
−7
d yr
−1
). This trend could be attributed to the angular momentum loss via stellar wind. |
---|---|
AbstractList | V0842 Cep is a W UMa-type binary star that has been neglected since its discovery. We analysed the VRcIc light curves, obtained by the 1 m telescope at Weihai Observatory of Shandong University, using the Wilson-Devinney code. V0842 Cep was found to be a shallow contact binary system (f = 8.7%) with a mass ratio of 2.281. Because its orbital inclination is greater than 80°, the photometric results are reliable. A period study is included which reveals a continually decreasing orbital period (\(\frac{{\rm{d}}p}{{\rm{d}}t}\) = 1.50(±0.42)×10−7 d yr−1). This trend could be attributed to the angular momentum loss via stellar wind. V0842 Cep is a W UMa-type binary star that has been neglected since its discovery. We analysed the VR c I c light curves, obtained by the 1 m telescope at Weihai Observatory of Shandong University, using the Wilson-Devinney code. V0842 Cep was found to be a shallow contact binary system ( f = 8.7%) with a mass ratio of 2.281. Because its orbital inclination is greater than 80°, the photometric results are reliable. A period study is included which reveals a continually decreasing orbital period ( d p d t = 1.50(±0.42)×10 −7 d yr −1 ). This trend could be attributed to the angular momentum loss via stellar wind. V0842 Cep is a W UMa-type binary star that has been neglected since its discovery.We analysed the VRcIc light curves,obtained by the 1 m telescope at Weihai Observatory of Shandong University,using the Wilson-Devinney code.V0842 Cep was found to be a shallow contact binary system(f=8.7%) with a mass ratio of 2.281.Because its orbital inclination is greater than 80°,the photometric results are reliable.A period study is included which reveals a continually decreasing orbital period(dp/dt=1.50(±0.42) × 10-7d yr-1).This trend could be attributed to the angular momentum loss via stellar wind. |
Author | Li, Kai Liu, Yuan Li, Yu-Yang |
AuthorAffiliation | Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment,Institute of Space Sciences,Shandong University,Weihai 264209,China%Qilu Institute of Technology,Jinan 250200,China |
AuthorAffiliation_xml | – name: Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment,Institute of Space Sciences,Shandong University,Weihai 264209,China%Qilu Institute of Technology,Jinan 250200,China |
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GrantInformation_xml | – fundername: This work is supported by the Joint Research Fund in Astronomy (Grant No.U1931103). under cooperative agreement between National Natural Science Foundation of China (NSFC) and Chinese Academy of Sciences (CAS),the NSFC ; (the Natural Science Foundation of Shandong Province ); (the Young Scholars Program of Shandong University,Weihai ); (the Chinese Academy of Sciences Interdisciplinary Innovation Team,and by the Open Research Program of Key Laboratory for the Structure and Evolution of Celestial Objects ); We would like to acknowledge the AAVSO International Database (https .//www.aavso.org/),from which variable star observations were obtained; Observers worldwide have contributed to this database; (Further,this article uses data from the All-Sky Automated Survey for SuperNovae ); which consists of two telescopes on a common mount and is hosted by the Las Cumbres Observatory Global Telescope Network in the Faulkes Telescope North enclosure on Mount Haleakala,Hawaii; Finally,this work has utilised data listed in the European Space Agency mission Gaia (https.//www.cosmos.esa.int/gaia),processed by the Gaia Data Processing and Analysis Consortium (DPAC.https .//www.cosmos.esa.int/web/gaia/dpac/consortium); Funding for the DPAC was provided by national institutions,in particular the institutions participating in the Gaia Multilateral Agreement; This work is partly supported by the Supercomputing Center of Shandong University,Weihai funderid: (Grant No.11703016); (the Natural Science Foundation of Shandong Province ); (the Young Scholars Program of Shandong University,Weihai ); (the Chinese Academy of Sciences Interdisciplinary Innovation Team,and by the Open Research Program of Key Laboratory for the Structure and Evolution of Celestial Objects ); We would like to acknowledge the AAVSO International Database (https .//www.aavso.org/),from which variable star observations were obtained; Observers worldwide have contributed to this database; (Further,this article uses data from the All-Sky Automated Survey for SuperNovae ); which consists of two telescopes on a common mount and is hosted by the Las Cumbres Observatory Global Telescope Network in the Faulkes Telescope North enclosure on Mount Haleakala,Hawaii; (ESA) mission Gaia (https.//www.cosmos.esa.int/gaia),processed by the Gaia Data Processing and Analysis Consortium (DPAC.https .//www.cosmos.esa.int/web/gaia/dpac/consortium); Funding for the DPAC was provided by national institutions,in particular the institutions participating in the Gaia Multilateral Agreement; This work is partly supported by the Supercomputing Center of Shandong University,Weihai |
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Snippet | V0842 Cep is a W UMa-type binary star that has been neglected since its discovery. We analysed the
VR
c
I
c
light curves, obtained by the 1 m telescope at... V0842 Cep is a W UMa-type binary star that has been neglected since its discovery. We analysed the VRcIc light curves, obtained by the 1 m telescope at Weihai... V0842 Cep is a W UMa-type binary star that has been neglected since its discovery.We analysed the VRcIc light curves,obtained by the 1 m telescope at Weihai... |
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StartPage | 122 |
SubjectTerms | Angular momentum Binary stars Light curve Orbits Photometry stars: binaries: close stars: binaries: eclipsing stars: individual (V0842 Cep) Stellar winds |
Title | The first photometric analysis and period investigation of the K-type W UMa type binary system V0842 Cep |
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