Type Ia supernovae are the result of explosive thermonuclear burning in CO white dwarfs. The progenitors of the Ia supernovae are white dwarfs in an interacting binary system. The donor companion is either a degenerate star (white dwarf) or a non-degenerate star (e.g. red giant). Recurrent novae are interacting binaries with a massive white dwarf accreting from either a main sequence, slightly evolved, or a red giant star. The white dwarf in these systems is a massive, hot white dwarf, accreting at a high rate. Recurrent novae are thought to be the most promising single degenerate progenitors of Type Ia supernovae. Presented here are the properties of a few recurrent novae based on recent outbursts. The elemental abundances and their distribution in the ejected shell are discussed.

中文翻译：

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复发新星：Ia 型超新星的单一退化前身

Ia 型超新星是 CO 白矮星中爆炸性热核燃烧的结果。Ia 超新星的前身是相互作用的双星系统中的白矮星。供体伴星要么是退化恒星（白矮星），要么是非退化恒星（例如红巨星）。循环新星是与一颗大质量白矮星相互作用的双星，该白矮星来自主序星、略微演化的恒星或红巨星。这些系统中的白矮星是一颗巨大的、炽热的白矮星，以很高的速度吸积。复发新星被认为是 Ia 型超新星最有希望的单一退化前身。这里介绍的是一些基于最近爆发的周期性新星的特性。讨论了喷射壳中的元素丰度及其分布。