Total eclipse of the heart: the AM CVn Gaia14aae/ASSASN-14cn-猫眼课题宝

DOI：

10.1093/mnras/stv1224

发表时间：

2015-07

期刊：

Monthly Notices of the Royal Astronomical Society

影响因子：

4.8

通讯作者：

中科院分区：

物理与天体物理2区

文献类型：

作者：

H. Campbell;T. Marsh;M. Fraser;S. Hodgkin;E. Miguel;B. Gansicke;D. Steeghs;A. Hourihane;E. Breedt;S. Littlefair;Sergey E. Koposov;L. Wyrzykowski;G. Altavilla;N. Blagorodnova;G. Clementini;G. Damljanovic;Antonio Delgado;M. Dennefeld;A. Drake;J. Fern'andez-Hern'andez;G. Gilmore;R. Gualandi;A. Hamanowicz;B. Handzlik;L. Hardy;D. Harrison;K. Iłkiewicz;P. Jonker;C. Kochanek;Z. Kołaczkowski;Z. Kostrzewa-Rutkowska;R. Kotak;G. V. Leeuwen;G. Leto;P. Ochner;M. Pawlak;L. Palaversa;G. Rixon;K. Rybicki;B. Shappee;S. Smartt;M. Torres;L. Tomasella;M. Turatto;K. Ulaczyk;S. Velzen;O. Vince;N. Walton;P. Wielg'orski;T. Wevers;P. Whitelock;A. Yoldas;F. Angeli;P. Burgess;G. Busso;R. Busuttil;T. Butterley;K. Chambers;C. Copperwheat;A. B. Danilet;V. Dhillon;D. Evans;L. Eyer;D. Froebrich;A. Gomboc;G. Holland;T. Holoien;J. Jarvis;N. Kaiser;D. A. Kann;D. Koester;U. Kolb;S. Komossa;E. Magnier;A. Mahabal;J. Polshaw;J. Prieto;T. Prusti;M. Riello;A. Scholz;G. Simonian;K. Stanek;L. Szabados;C. Waters;R. Wilson

我们报道了一个深食AM CVn系统Gaia 14 aae（=ASSASN-14 cn）的发现和特征。Gaia 14 aae是由全天空超新星自动巡天（ASAS-SN; Shappee et al.）和盖亚科学警报项目，在两个独立的爆发。第三次爆发是在档案Pan-STARRS-1中看到的（PS1; Schlafly et al.; Tendon等人; Magnier等人）ASAS-SN数据光谱揭示了一个热，氢缺乏光谱与明确的双峰发射线，符合吸积双简并分类。我们使用跟踪测光来约束系统的轨道参数。我们发现一个轨道周期为49.71分钟，这地方Gaia 14 aae在爆发AM CVn周期分布的长周期极值。Gaia 14 aae主要由其吸积的白色矮星（WD）发出的光所控制。假设双星系统的轨道倾角为90°，WD的接触相导致吸积体和施主的质量下限分别为0.78和0.015 M，质量比下限为0.019。Gaia 14 aae是已知的第三颗食AM CVn的星星，也是第一颗被WD完全食的恒星。用氦WD模型估算了吸积体的有效温度为12900 ± 200 K。这三次爆发事件发生在四个月内，而在过去8年的卡塔利纳实时瞬时调查（CRTS; Drake等人）中没有发现其他爆发活动，Pan-STARRS-1和ASAS-SN数据。这表明，这些事件可能是第一次爆发的重新亮化，而不是个别事件。

We report the discovery and characterization of a deeply eclipsing AM CVn-system, Gaia14aae (=ASSASN-14cn). Gaia14aae was identified independently by the All-Sky Automated Survey for Supernovae (ASAS-SN; Shappee et al.) and by the Gaia Science Alerts project, during two separate outbursts. A third outburst is seen in archival Pan-STARRS-1 (PS1; Schlafly et al.; Tonry et al.; Magnier et al.) and ASAS-SN data. Spectroscopy reveals a hot, hydrogen-deficient spectrum with clear double-peaked emission lines, consistent with an accreting double-degenerate classification. We use follow-up photometry to constrain the orbital parameters of the system. We find an orbital period of 49.71 min, which places Gaia14aae at the long period extremum of the outbursting AM CVn period distribution. Gaia14aae is dominated by the light from its accreting white dwarf (WD). Assuming an orbital inclination of 90° for the binary system, the contact phases of the WD lead to lower limits of 0.78 and 0.015 M⊙ on the masses of the accretor and donor, respectively, and a lower limit on the mass ratio of 0.019. Gaia14aae is only the third eclipsing AM CVn star known, and the first in which the WD is totally eclipsed. Using a helium WD model, we estimate the accretor's effective temperature to be 12 900 ± 200 K. The three outburst events occurred within four months of each other, while no other outburst activity is seen in the previous 8 yr of Catalina Real-time Transient Survey (CRTS; Drake et al.), Pan-STARRS-1 and ASAS-SN data. This suggests that these events might be rebrightenings of the first outburst rather than individual events.

Total eclipse of the heart: the AM CVn Gaia14aae/ASSASN-14cn

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