矮新星的距离和绝对星等：周期反弹的杂音
Distances and Absolute Magnitudes of Dwarf Novae: Murmurs of Period Bounce
摘要：
我们重新确定的绝对星等和矮新星的轨道周期之间的关系，基于46颗恒星良好的距离估计。这改进了华纳以前的关系，建立在今天的距离和双星倾角的改进估计，以及更大的波长覆盖范围。结合其他距离和动力学约束条件，将该定标应用于一组约300颗已知或可能的短轨道周期矮新星，研究了静止M_v、时间平均M_v、质量比q和白矮星温度T_WD对P_orb的依赖关系。这些分布表明，当恒星接近最小P_orb时，它们会变得更加暗淡，并且似乎显示出/进化轨迹/，因为次级恒星因质量损失而减弱。在较低的分支上的恒星具有“周期跳跃者”的预期特性--微弱的次级，微弱的吸积光，冷的白矮星，以及爆发之间的长重复时间。周期反弹似乎发生在0.058+-0.008 M_sol的质量。在较低分支的恒星也可能有较高的速度和银河平面以上的高度，与更大的年龄相一致。一些非常接近，尽管强烈的选择效应歧视这些微弱的双星的发现，以非常低的速度吸积。周期保镖似乎很常见，可能会主导一个完整的普查灾难性的变量。
英文摘要：
We redetermine the relationship between absolute magnitude and orbital period for dwarf novae, based on 46 stars with good distance estimates. This improves upon Warner's previous relation, building upon today's improved estimates of distance and binary inclination, and greater wavelength coverage. Together with other distance and dynamical constraints, this calibration is then applied to a set of ~300 known or likely dwarf novae of short orbital period, to study the dependence of quiescent M_v, time-averaged M_v, mass ratio q, and white-dwarf temperature T_WD, on P_orb. These distributions show that stars become much fainter as they approach minimum P_orb, and appear to show /evolutionary tracks/ as the secondary is whittled down by mass loss. Stars on the lower branch have the expected properties of "period bouncers" -- with a feeble secondary, faint accretion light, cool white dwarf, and long recurrence time between eruptions. Period bounce seems to occur at a mass of 0.058+-0.008 M_sol. Stars on the lower branch may also have higher velocities and heights above the Galactic plane, consistent with a greater age. Some are very nearby, despite strong selection effects discriminating against the discovery of these faint binaries accreting at very low rates. Period bouncers appear to be very common, and probably would dominate a complete census of cataclysmic variables.
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