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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
Source PublicationASTRONOMICAL JOURNAL
2018-10-01
Volume156Issue:4Pages:17
DOI10.3847/1538-3881/aadb99
Indexed BySCI
Keywordbinaries (including multiple): close novae, cataclysmic variables white dwarfs
Abstract

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.

Funding ProjectCAS 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
Funding OrganizationCAS Light of West China Program ; Chinese Natural Science Foundation[11133007, 11325315] ; Science Foundation of Yunnan Province[2016FB007] ; NSF[AST-1514737] ; Royal Society ; Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences
Language英语
Subject Area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
ISSN0004-6256
URL查看原文
WOS IDWOS:000444462300004
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS KeywordX-RAY BINARIES ; ACCRETION DISKS ; WHITE-DWARFS ; RZ LEONIS ; BOLOMETRIC CORRECTIONS ; EFFECTIVE TEMPERATURES ; Z-CHAMAELEONTIS ; MASS-RADIUS ; SPACED DATA ; HOT-SPOT
Citation statistics
Document Type期刊论文
Identifierhttp://ir.ynao.ac.cn/handle/114a53/17908
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 AuthorDai ZB(戴智斌)
Affiliation1.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
First Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Corresponding Author AffilicationYunnan Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
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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