新星V458 Vul周围的行星状星云正在经历闪光电离
A planetary nebula around nova V458 Vul undergoing flash ionization
摘要：
新星V458 Vul于2007年8月8日爆发，几天后达到8.1等。作为IPHAS银道面巡天的一部分，在爆发前六周获得的H $α$图像显示了一个被扩展星云包围的18等祖先。随后的图像和星云光谱显示，由于新星事件的闪光电离，星云内部的一个结的亮度迅速增加。我们推导出的距离为13千秒差距的基础上光的旅行时间的考虑，这是由其他两个距离估计方法的支持。该星云的电离质量为0.2 M $_{\odot}$，膨胀速度较低：这排除了它是之前新星喷发的喷出物，并与它是一个约14，000年前的行星状星云相一致，可能是双星系统演化过程中先前的共同包络（CE）阶段的产物。大的派生距离意味着爆发的WD组件的二进制的质量是高的。我们确定了两种可能的进化方案，其中至少有一个系统的质量足以产生一个Ia型超新星合并。
英文摘要：
Nova V458 Vul erupted on 2007 August 8th and reached a visual magnitude of 8.1 a few days later. H$α$ images obtained six weeks before the outburst as part of the IPHAS galactic plane survey reveal an 18th magnitude progenitor surrounded by an extended nebula. Subsequent images and spectroscopy of the nebula reveal an inner nebular knot increasing rapidly in brightness due to flash ionization by the nova event. We derive a distance of 13 kpc based on light travel time considerations, which is supported by two other distance estimation methods. The nebula has an ionized mass of 0.2 M$_{\odot}$ and a low expansion velocity: this rules it out as ejecta from a previous nova eruption, and is consistent with it being a ~14,000 year old planetary nebula, probably the product of a prior common envelope (CE) phase of evolution of the binary system. The large derived distance means that the mass of the erupting WD component of the binary is high. We identify two possible evolutionary scenarios, in at least one of which the system is massive enough to produce a Type Ia supernova on merging.
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