A Phenomenological Model for the Light Curve of three Quiescent Low-inclination Dwarf Novae and one Pre-Cataclysmic Variable

• 作者： Dai, zhibin ( 1,2,3,4,5 ) ; Szkody, Paula ( 6 ) ; Kennedy, Mark ( 7 ) ; Su Jie ( 1,2,4 ) ; Medagangoda, N. Indika ( 8 ) ; Robinson, Edward L. ( 9 ) ; Garnavich, Peter M. ( 10 ) ; De Silva, L. Malith M. ( 11 ) ;
• 作者单位： 1.Yunnan Observatories, Chinese Academy of Sciences, 396 Yangfangwang, Guandu District, Kunming, 650216, P. R. China.; 2.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, 396 Yangfangwang, Guandu District, Kunming, 650216, P. R. 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, P. R. China.; 5.University of Chinese Academy of Sciences, No.19(A) Yuquan Road, Shijingshan District, Beijing, 100049, P.R.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.;
• 提交时间：2018-09-12

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 $\sim0.11$. 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.

• 来自： zhibin_dai@ynao.ac.cn
• 主题： Cataclysmic Variables, White Dwarf, Synthetic method
• 期刊： The Astronomy Journal
• 分类： 天文学 >> 天体物理学 天文学 >> 恒星和银河系
• 引用： ChinaXiv:201808.00172 (或此版本 ChinaXiv:201808.00172V2)
  (doi:10.12074/201808.00172)
  (CSTR:32003.36.ChinaXiv.201808.00172.V1)
• 推荐引用方式：Dai, zhibin,Szkody, Paula,Kennedy, Mark,Su Jie,Medagangoda, N. Indika,Robinson, Edward L.,Garnavich, Peter M.,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.The Astronomy Journal.CSTR:32003.36.ChinaXiv.201808.00172.V2 (点此复制)