论文标题
Lamost发现的五个灾难性可变候选者的后续研究
Follow-up Studies of Five Cataclysmic Variable Candidates Discovered by LAMOST
论文作者
论文摘要
我们报告了Hou等人发表的Lamost的五个灾难性可变候选者的随访观察结果。 （2020）。 Lamost J024048.51+195226.9是五个中最不寻常的；早期M型二级恒星对其光谱有很大贡献，其光谱和光度法极大地让人联想到迄今唯一的螺旋桨系统AE AQR。我们确认在Catalina调查数据中发现了7.34小时（Drake等人，2014年）是轨道。另一个对象是Lamost J204305.95+341340.6似乎是Novalike变量V795她的近二元，在所谓的2-3小时“差距”中有轨道时期。 Lamost J035913.61+405035.0显然是一个黯然失色的，弱的矮人矮人Nova，其时间为5.48 hr。我们的Lamost J090150.09+375444.3的光谱以后期型次级为主，显示出弱，狭窄的Balmer发射与吸收线相相移，但幅度较低。我们看不到已发表的发现范围中发现的HEII 4686排放。我们再次确认来自Catalina数据（在这种情况下为6.80小时）的时期是轨道。 Lamost J033940.98+414805.7产生的径向速度周期为3.54小时，其频谱似乎在此期间范围内是Novalike变量的典型代表。来自LAMOST的光谱式选择样品显然包括一些有趣的灾难性变量，这些变量迄今尚未被识别，这显然是因为它们的光度变化的相对适度范围。
We report follow-up observations of five cataclysmic variable candidates from LAMOST published by Hou et al. (2020). LAMOST J024048.51+195226.9 is the most unusual of the five; an early-M type secondary star contributes strongly to its spectrum, and its spectral and photometric behavior are strikingly reminiscent of the hitherto-unique propeller system AE Aqr. We confirm that a 7.34-hr period discovered in the Catalina survey data (Drake et al. 2014) is orbital. Another object, LAMOST J204305.95+341340.6 appears to be a near twin of the novalike variable V795 Her, with an orbital period in the so-called 2-3 hour "gap". LAMOST J035913.61+405035.0 is evidently an eclipsing, weakly-outbursting dwarf nova with a 5.48-hr period. Our spectrum of LAMOST J090150.09+375444.3 is dominated by a late-type secondary and shows weak, narrow Balmer emission moving in phase with the absorption lines, but at lower amplitude; we do not see the HeII 4686 emission evident in the published discovery spectrum. We again confirm that a period from the Catalina data, in this case 6.80 hr, is orbital. LAMOST J033940.98+414805.7 yields a radial-velocity period of 3.54 hr, and its spectrum appears to be typical of novalike variables in this period range. The spectroscopically-selected sample from LAMOST evidently includes some interesting cataclysmic variables that have been unrecognized until now, apparently because of the relatively modest range of their photometric variations.
