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首页> 外文期刊>Astronomy and astrophysics >The 2014–2017 outburst of the young star ASASSN-13db - A time-resolved picture of a very-low-mass star between EXors and FUors
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The 2014–2017 outburst of the young star ASASSN-13db - A time-resolved picture of a very-low-mass star between EXors and FUors

机译：2014-2017年年轻恒星ASASSN-13db的爆发-时间分辨的照片是EXor和FUors之间极低质量的恒星

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Context. Accretion outbursts are key elements in star formation. ASASSN-13db is a M5-type star with a protoplanetary disk, the lowest-mass star known to experience accretion outbursts. Since its discovery in 2013, it has experienced two outbursts, the second of which started in November 2014 and lasted until February 2017. Aims. We explore the photometric and spectroscopic behavior of ASASSN-13db during the 2014–2017 outburst. Methods. We use high- and low-resolution spectroscopy and time-resolved photometry from the ASAS-SN survey, the LCOGT and the Beacon Observatory to study the light curve of ASASSN-13db and the dynamical and physical properties of the accretion flow. Results. The 2014–2017 outburst lasted for nearly 800 days. A 4.15 d period in the light curve likely corresponds to rotational modulation of a star with hot spot(s). The spectra show multiple emission lines with variable inverse P-Cygni profiles and a highly variable blue-shifted absorption below the continuum. Line ratios from metallic emission lines (Fe I/Fe II, Ti I/Ti II) suggest temperatures of ~ 5800–6000 K in the accretion flow. Conclusions. Photometrically and spectroscopically, the 2014–2017 event displays an intermediate behavior between EXors and FUors. The accretion rate ([ ? ]=?1– 3 × 10~(-7) M _(⊙) /yr), about two orders of magnitude higher than the accretion rate in quiescence, is not significantly different from the accretion rate observed in 2013. The absorption features in the spectra suggest that the system is viewed at a high angle and drives a powerful, non-axisymmetric wind, maybe related to magnetic reconnection. The properties of ASASSN-13db suggest that temperatures lower than those for solar-type stars are needed for modeling accretion in very-low-mass systems. Finally, the rotational modulation during the outburst reveals that accretion-related structures settle after the beginning of the outburst and can be relatively stable and long-lived. Our work also demonstrates the power of time-resolved photometry and spectroscopy to explore the properties of variable and outbursting stars.
机译：上下文。吸积爆发是恒星形成的关键因素。 ASASSN-13db是一颗M5型恒星，带有一个原行星盘，这是质量最低的恒星，已知会经历增生爆发。自2013年被发现以来，它经历了两次爆发，第二次爆发于2014年11月开始，一直持续到2017年2月。我们探讨了2014-2017年爆发期间ASASSN-13db的光度学和光谱学行为。方法。我们使用ASAS-SN调查，LCOGT和信标天文台的高分辨率和低分辨率光谱学和时间分辨光度法研究了ASASSN-13db的光曲线以及吸积流的动态和物理特性。结果。 2014-2017年爆发持续了将近800天。光曲线中的4.15 d周期可能对应于具有热点的恒星的旋转调制。光谱显示多条发射线具有可变的反向P-Cygni轮廓，并且在连续峰以下具有高度可变的蓝移吸收。金属排放管线的线比（Fe I / Fe II，Ti I / Ti II）表明，吸积流中的温度约为5800–6000K。结论。用光度法和分光镜，2014–2017年的事件显示了EXor和FUor之间的中间行为。吸积率（[？] =？1-3×10〜（-7）M _（⊙）/ yr）比静止时的吸积率高约两个数量级，与观察到的吸积率没有显着差异在2013年。光谱中的吸收特征表明，从高角度观察该系统会产生强大的非轴对称风，这可能与磁重联有关。 ASASSN-13db的性质表明，在极低质量的系统中对积聚进行建模时，需要温度低于太阳型恒星的温度。最后，爆发过程中的旋转调制表明，与爆发相关的结构在爆发开始后就稳定下来了，并且相对稳定且寿命长。我们的工作还证明了时间分辨光度法和光谱法探索变星和爆发星的特性的能力。

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