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RAPID DECREASING IN THE ORBITAL PERIOD OF THE DETACHED WHITE DWARF-MAIN SEQUENCE BINARY SDSS J143547.87+373338.5
Qian SB(钱声帮)1,2,3; Han ZT(韩忠涛)1,2,3; Soonthornthum, B.4; Zhu LY(朱俐颖)1,2,3; He JJ(何家佳)1,2; Rattanasoon, S.4; Aukkaravittayapun, S.4; Liao WP(廖文萍)1,2; Zhao EG(赵二刚)1,2,3; Zhang J(张嘉)1,2; Fernandez Lajus, E.5,6,7
Source PublicationASTROPHYSICAL JOURNAL
2016-02-01
Volume817Issue:2
DOI10.3847/0004-637X/817/2/151
Contribution Rank第1完成单位
Indexed BySCI
KeywordBinaries: Close Binaries: Eclipsing Brown Dwarfs Stars: Individual (Sdss j143547.87+373338.5) Stars: Low-mass White Dwarfs
Abstract

SDSS J143547.87+373338.5 is a detached eclipsing binary that contains a white dwarf with a mass of 0.5 M-circle dot and a fully convective star with a mass of 0.21 M-circle dot. The eclipsing binary was monitored photometrically from 2009 March 24 to 2015 April 10, by using two 2.4-m telescopes in China and in Thailand. The changes in the orbital period are analyzed based on eight newly determined eclipse times together with those compiled from the literature. It is found that the observed-calculated (O-C) diagram shows a downward parabolic change that reveals a continuous period decrease at a rate of (P) over dot = -8.04 x 10(-11) s s(-1). According to the standard theory of cataclysmic variables, angular momentum loss (AML) via magnetic braking (MB) is stopped for fully convective stars. However, this period decrease is too large to be caused by AML via gravitational radiation (GR), indicating that there could be some extra source of AML beyond GR, but the predicted mass-loss rates from MB seem unrealistically large. The other possibility is that the O-C diagram may show a cyclic oscillation with a period of 7.72 years and a small amplitude of 0.(d)000525. The cyclic change can be explained as the light-travel-time effect via the presence of a third body because the required energy for the magnetic activity cycle is much larger than that radiated from the secondary in a whole cycle. The mass of the potential third body is determined to be M-3 sin t' = 0.0189(+/- 0.0016) M-circle dot when a total mass of 0.71 M-circle dot for SDSS J143547.87+ 373338.5 is adopted. For orbital inclinations i' >= 15.degrees 9, it would be below the stable hydrogen-burning limit of M-3 similar to 0.072 M-circle dot, and thus the third body would be a brown dwarf.

Funding ProjectChinese Natural Science Foundation [11133007] ; Chinese Natural Science Foundation [11325315] ; Key Research Program of the Chinese Academy of Sciences[KGZD-EW-603] ; Science Foundation of Yunnan Province [2012HC011] ; Science Foundation of Yunnan Province [2013FB084] ; Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences[XDB09010202]
Funding OrganizationChinese Natural Science Foundation [11133007, 11325315] ; Key Research Program of the Chinese Academy of Sciences[KGZD-EW-603] ; Science Foundation of Yunnan Province [2012HC011, 2013FB084] ; Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences[XDB09010202]
Language英语
Subject Area天文学 ; 恒星与银河系 ; 恒星天文学
MOST Discipline Catalogue理学 ; 理学::天文学
SubtypeArticle
PublisherIOP PUBLISHING LTD
Publication PlaceTEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
ISSN0004-637X
URL查看原文
Archive Date2016-04-12
WOS IDWOS:000369437900068
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordCOMMON-ENVELOPE BINARIES ; VIRGINIS PLANETARY SYSTEM ; BROWN-DWARF ; MAGNETIC BRAKING ; CIRCUMBINARY DISKS ; NN-SER ; HU AQR ; COMPANION ; EVOLUTION ; TEMPERATURE
Citation statistics
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/9331
Collection双星与变星研究组
中国科学院天体结构与演化重点实验室
Corresponding AuthorQian SB(钱声帮)
Affiliation1.Yunnan Observatories, Chinese Academy of Sciences (CAS), P.O. Box 110, 650011 Kunming, P. R. China
2.Key Laboratory of the Structure and Evolution Celestial Bodies, Chinese Academy of Sciences, P.O. Box 110, 650011 Kunming, P. R. China
3.University of the Chinese Academy of Sciences, Yuquan Road 19#, Sijingshang Block, 100049 Beijing, P. R. China
4.National Astronomical Research Institute of Thailand, 191 Siriphanich Bldg., Huay Kaew Rd., Chiang Mai 50200, Thailand
5.Facultad de Ciencias Astronómicas y Geofiísicas, Universidad Nacional de La Plata, 1900 La Plata, Buenos Aires, Argentina
6.Instituto de Astrofisica de La Plata (CCT La plata—CONICET/UNLP), Argentina
7.Visiting Astronomer, Complejo Astronómico El Leoncito operated under agreement between the Consejo Nacional de Investigaciones Científicas y Técnicas de la República Argentina and the National Universities of La Plata, Córdoba and San Juan.
First Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Corresponding Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
Qian SB,Han ZT,Soonthornthum, B.,et al. RAPID DECREASING IN THE ORBITAL PERIOD OF THE DETACHED WHITE DWARF-MAIN SEQUENCE BINARY SDSS J143547.87+373338.5[J]. ASTROPHYSICAL JOURNAL,2016,817(2).
APA Qian SB.,Han ZT.,Soonthornthum, B..,Zhu LY.,He JJ.,...&Fernandez Lajus, E..(2016).RAPID DECREASING IN THE ORBITAL PERIOD OF THE DETACHED WHITE DWARF-MAIN SEQUENCE BINARY SDSS J143547.87+373338.5.ASTROPHYSICAL JOURNAL,817(2).
MLA Qian SB,et al."RAPID DECREASING IN THE ORBITAL PERIOD OF THE DETACHED WHITE DWARF-MAIN SEQUENCE BINARY SDSS J143547.87+373338.5".ASTROPHYSICAL JOURNAL 817.2(2016).
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