论文标题
对30个短期灾难性可变星的光谱研究，并就相似物体的进化和种群进行评论
Spectroscopic Studies of 30 Short-period Cataclysmic Variable Stars, and Remarks on the Evolution and Population of Similar Objects
论文作者
论文摘要
我们在30个显然是非磁性灾难性的二进制物中，呈现光谱和轨道周期，其周期低于3小时，几乎所有的都是矮人Novae，主要是Su Ursae Majoris子类。然后，我们求助于支持以下预测的证据，即短期矮化的novae在经过最低时期后朝着更长的时期发展 - “时期反弹”现象。从文献中绘制数据表明，对于超值期，$ε=（p _ {\ rm sh} - p _ {\ rm orb}）/p _ {\ rm orb} $以下低于0.015，该周期似乎随着epsilon而下降，至少在质量上同意了预测的行为。接下来，以短期矮人矮人的WZ Sagittae子类的长时间爆发间隔的激励，我们询问是否可能存在相当大的“潜伏者”人群 - 类似于矮人的系统，以最少的光线，但不会在可访问的时代（或根本不引起您的注意力）上，并且没有引起人们的注意。通过检查Sloan数字天空调查CVS的爆发历史，这些样本是通过颜色而不是爆发选择的，我们发现，已经观察到了大部分颜色选择的矮人型矮人，并且已经爆发了，并得出结论，“ Lurkers”（如果存在的话）是相对较小的CV群体的一部分。
We present spectroscopy and orbital periods Porb for 30 apparently non-magnetic cataclysmic binaries with periods below about 3 hours, nearly all of which are dwarf novae, mostly of the SU Ursae Majoris subclass. We then turn to the evidence supporting the prediction that short-period dwarf novae evolve toward longer periods after passing through a minimum period -- the "period bounce" phenomenon. Plotting data from the literature reveals that for superhump period excess $ε= (P_{\rm sh} - P_{\rm orb} )/P_{\rm orb}$ below about 0.015, the period appears to increase with decreasing epsilon, agreeing at least qualitatively with the predicted behavior. Next, motivated by the long (decadal) outburst intervals of the WZ Sagittae subclass of short-period dwarf novae, we ask whether there could be a sizable population of "lurkers" -- systems that resemble dwarf novae at minimum light, but do not outburst over accessible timescales (or at all), and therefore do not draw attention to themselves. By examining the outburst history of the Sloan Digital Sky Survey sample of CVs, which were selected by color and not by outburst, we find that a large majority of the color-selected dwarf-nova-like objects have been observed to outburst, and conclude that "lurkers", if they exist, are a relatively minor part of the CV population.
