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A Phenomenological Model for the Light Curve of Three Quiescent Low-inclination Dwarf Novae and One Pre-cataclysmic Variable
Dai ZB(戴智斌)1,2,3,4,5; Szkody, Paula6; Kennedy, Mark7; Su J(苏杰)1,2,4; Medagangoda, N. Indika8; Robinson, Edward L.9; Garnavich, Peter M.10; De Silva, L. Malith M.11
通讯作者Dai, Zhibin(zhibin_dai@ynao.ac.cn)
发表期刊ASTRONOMICAL JOURNAL
2018-10-01
卷号156期号:4页码:17
DOI10.3847/1538-3881/aadb99
收录类别SCI
关键词binaries (including multiple): close novae, cataclysmic variables white dwarfs
摘要We used the light curve code XRBinary to model the quiescent K2 light curves of three low-inclination cataclysmic variables (CVs): 1RXS J0632+2536 (J0632+2536), RZ Leo, TW Vir and the pre-CV WD 1144+011. Optimized light curve models were obtained using a nonlinear fitting code NMfit and visualized by Phoebe 2.0. The disk model of J0632+2536 shows that one hotspot at the edge of the disk is enough to describe its light curve, while the other two dwarf nova (DN): RZ Leo and TW Vir require two hotspots. A typical pre-CV model with a weak irradiation effect for WD 1144+011 can explain its single-hump modulation and the newly observed spectrum confirms its previous classification. The synthetic analyses for the DN clearly indicate that phase zero of the double-hump modulations occurs around the secondary minimum and the primary hump is mainly caused by the hotspot at the edge of the disk. The quiescent disk has a flat temperature distribution with a power index of -0.11. The disk model of RZ Leo implies a truncated disk, supporting its previously speculated classification as an intermediate polar (IP). Except for the IP model of RZ Leo, which lacks a component related to the inferred accretion curtain, the models of J0632+2536, TW Vir and WD 1144+011 are consistent with results from the Gaia mission. The derived masses and radii of the secondaries of the three DN are consistent with the semi-empirical relations for CV donor stars, while their effective temperatures are higher than the predictions. Irradiation of the donor stars is investigated to explain this discrepancy.
资助项目CAS Light of West China Program ; Chinese Natural Science Foundation[11133007] ; Chinese Natural Science Foundation[11325315] ; Science Foundation of Yunnan Province[2016FB007] ; NSF[AST-1514737] ; Royal Society ; Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences
项目资助者CAS Light of West China Program ; Chinese Natural Science Foundation ; Science Foundation of Yunnan Province ; NSF ; Royal Society ; Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences
语种英语
学科领域天文学
学科门类理学 ; 理学::天文学
文章类型Article
出版者IOP PUBLISHING LTD
ISSN0004-6256
URL查看原文
WOS记录号WOS:000444462300004
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]X-RAY BINARIES ; ACCRETION DISKS ; WHITE-DWARFS ; RZ LEONIS ; BOLOMETRIC CORRECTIONS ; EFFECTIVE TEMPERATURES ; Z-CHAMAELEONTIS ; MASS-RADIUS ; SPACED DATA ; HOT-SPOT
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文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/17908
专题双星与变星研究组
中国科学院天体结构与演化重点实验室
通讯作者Dai ZB(戴智斌)
作者单位1.Yunnan Observatories, Chinese Academy of Sciences, 396 Yangfangwang, Guandu District, Kunming, 650216, People's Republic of China
2.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, 396 Yangfangwang, Guandu District, Kunming, 650216, People's Republic of China
3.Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People's Republic of China
4.Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing, 100012, People's Republic of China
5.University of Chinese Academy of Sciences, No.19(A) Yuquan Road, Shijingshan District, Beijing, 100049, People's Republic of China
6.University of Washington, Seattle, WA, 98195, USA
7.Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester M13 9PL, UK
8.Arthur C. Clarke Institute for Modern Technologies, Sri Lanka
9.University of Texas at Austin, Austin, TX, USA
10.University of Notre Dame, Notre Dame, IN, 46556, USA
11.Sabaragamuwa University of Sri Lanka, Sri Lanka
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Dai ZB,Szkody, Paula,Kennedy, Mark,et al. A Phenomenological Model for the Light Curve of Three Quiescent Low-inclination Dwarf Novae and One Pre-cataclysmic Variable[J]. ASTRONOMICAL JOURNAL,2018,156(4):17.
APA Dai ZB.,Szkody, Paula.,Kennedy, Mark.,Su J.,Medagangoda, N. Indika.,...&De Silva, L. Malith M..(2018).A Phenomenological Model for the Light Curve of Three Quiescent Low-inclination Dwarf Novae and One Pre-cataclysmic Variable.ASTRONOMICAL JOURNAL,156(4),17.
MLA Dai ZB,et al."A Phenomenological Model for the Light Curve of Three Quiescent Low-inclination Dwarf Novae and One Pre-cataclysmic Variable".ASTRONOMICAL JOURNAL 156.4(2018):17.
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