经典新星中的CNO“爆发”与核合成
CNO "Breakout" and Nucleosynthesis in Classical Novae
摘要：
对于非常慢的白矮星吸积体，CV的Townsley和Bildsten（2004）发现了吸积速率和白矮星中心温度Tc之间的关系。根据这个关系式，当吸积速率小于10^-10太阳质量/年时，Tc远低于10 ^7 K。受这项研究的启发，我们跟踪了Tc低于10^7 K的大质量白矮星（M_WD=1.25 - 1.40太阳质量）上的热核逃逸，吸积了太阳成分的物质。我们证明，在相关参数空间（Tc、M_WD和吸积率）的范围内，失控过程中达到的峰值温度与Tc之间的关系的斜率比Tc高于10^7 K时的值要陡得多。我们推导出的峰值温度可以导致传统的“热碳-氮-氧”循环的核爆发。当突破条件实现时，重元素丰度可以显示出比普通富集机制可能的更广泛的变化。
英文摘要：
For very slow white dwarf accretors in CV's Townsley and Bildsten (2004) found a relation between the accretion rate and the central temperature of the white dwarf Tc. According to this relation for accretion rates less than 10^-10 solar masses per year Tc is much lower than 10^7 K. Motivated by this study we follow the thermonuclear runaway on massive white dwarfs (M_WD=1.25 - 1.40 solar masses) with Tc lower than 10^7 K, accreting matter of solar composition. We demonstrate that in that range of the relevant parameter space (Tc,M_WD and accretion rate) the slope of the relation between the peak temperatures achieved during the runaway and Tc becomes much steeper than its value for Tc above 10^7 K. The peak temperatures we derive can lead to nuclear breakout from the conventional "hot carbon-nitrogen-oxygen" cycle. When breakout conditions are achieved the heavy element abundances can show a much wider variety than what is possible with the common enrichment mechanisms.
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