Levitan等人最近的工作扩展了AM CVn星的长期光度数据库。特别是，它们的爆发特性与轨道周期密切相关，如果采用盘不稳定性模型进行爆发，则可以对次级和初级之间的长期传质速率进行约束。我们利用观测到的AM CVn系统爆发行为的范围作为轨道周期的函数，对质量转移速率与轨道周期P的关系进行限制。我们推断速率约为5 x 10^{-9} Msun/yr（P/1000 s）^{-5.2}。我们表明，这样得到的函数形式是一致的复发时间轨道周期关系发现Levitan等人使用一个简单的理论复发时间。此外，我们预测，一旦更长的轨道周期系统有更完整的观测，它们的爆发持续时间对轨道周期的陡峭依赖将大大平坦化。
英文摘要：
Recent work by Levitan et al has expanded the long-term photometric database for AM CVn stars. In particular, their outburst properties are well-correlated with orbital period, and allow constraints to be placed on the secular mass transfer rate between secondary and primary if one adopts the disk instability model for the outbursts. We use the observed range of outbursting behavior for AM CVn systems as a function of orbital period to place a constraint on mass transfer rate versus orbital period P. We infer a rate ~5 x 10^{-9} Msun/yr (P/1000 s)^{-5.2}. We show the functional form so obtained is consistent with the recurrence time-orbital period relation found by Levitan et al using a simple theory for the recurrence time. Also, we predict their steep dependence of outburst duration on orbital period will flatten considerably once the longer orbital period systems have more complete observations.
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