标题： Ia型超新星的起源：具有白矮星伴星的双星系统 显示英文标题

标题： Progenitors of Type Ia Supernovae: Binary Stars with White Dwarf Companions

摘要： Ia型超新星（SNe Ia）被认为来源于碳氧白矮星，这些白矮星从双星伴星吸积质量，直到接近钱德拉塞卡极限，点燃碳，并经历完全的热核瓦解。 本文综述了包含白矮星的观测到的各种双星系统。 我们建议，对于那些看起来最有可能作为SNe Ia前身天体的系统，应该更加密集地进行观测和建模，以确定这些系统中的白矮星是否能够达到钱德拉塞卡极限。 鉴于单简并系统数量众多而双简并系统缺乏的情况，我们怀疑单简并系统产生大多数甚至所有SNe Ia，而双简并系统则产生一些甚至没有产生任何SNe Ia。 显示英文摘要

摘要： Type Ia SNe (SNe Ia) are thought to come from carbon-oxygen white dwarfs that accrete mass from binary companions until they approach the Chandrasekhar limit, ignite carbon, and undergo complete thermonuclear disruption. A survey of the observed types of binaries that contain white dwarfs is presented. We propose that certain systems that seem most promising as SN Ia progenitors should be more intensively observed and modeled, to determine whether the white dwarfs in these systems will be able to reach the Chandrasekhar limit. In view of the number of promising single-degenerate systems and the dearth of promising double-degenerate systems, we suspect that single-degenerates produce most or perhaps all SNe Ia, while double-degenerates produce some or perhaps none.