论文标题
IA型超新星的前探索前氦壳闪光灯
Pre-explosion helium shell flash in type Ia supernovae
论文作者
论文摘要
我研究了IA型超新星（SNE IA）核心退化（CD）场景的可能性，渐近巨型分支（AGB）恒星（AGB）恒星的核心合并过程和白色矮人（WD）保持了〜0.03mo的质量，导致了〜0.03mo，这会导致后来的硫壳闪光灯。我估计，预探索前氦壳闪光事件的数量少于所有CD场景中的每美分。当恒星以后agb恒星（晚期脉冲； LTP）或沿WD冷却轨道（非常LTP）沿HR图的左侧移动时，氦壳闪光灯闪烁，使恒星扩展并成为重生的AGB恒星。合并残余物在仍处于AGB形式的同时爆炸{氢污染}奇特的sne ia，而在膨胀的重生恒星内的爆炸导致SN IA的光曲线的早期通量过量。由于LTP/VLTP而可能显示出早期通量过量的系统的比例为<（少数）X10^{ - 4}，远低于观察到的分数。在CD方案的框架中，SNE IA具有早期通量过量，导致Sn射流与行星星云后卫气体碰撞，或从56NI混合到Sn ejecta的外部区域。正在进行的天空调查可能会发现每年有LTP/VLTP影响SN光曲线的情况。
I study the possibility that within the frame of the core degenerate (CD) scenario for type Ia supernovae (SNe Ia) the merger process of the core of the asymptotic giant branch (AGB) star and the white dwarf (WD) maintains an envelope mass of ~0.03Mo that causes a later helium shell flash. I estimate the number of pre-explosion helium shell flash events to be less than few per cents of all CD scenario SNe Ia. A helium shell flash while the star moves to the left on the HR diagram as a post-AGB star (late thermal pulse; LTP) or along the WD cooling track (very LTP) causes the star to expand and become a born again AGB star. Merger remnants exploding while still on the AGB form {hydrogen-polluted} peculiar SNe Ia, while an explosion inside an inflated born-again star results in an early flux excess in the light curve of the SN Ia. The fraction of systems that might show an early flux excess due to LTP/VLTP is <(few)x10^{-4} of all SNe Ia, much below the observed fraction. In the frame of the CD scenario SNe Ia with early flux excess result from SN ejecta collision with planetary nebula fallback gas, or from mixing of 56Ni to the outer regions of the SN ejecta. Ongoing sky surveys might find about one case per year where LTP/VLTP influences the SN light curve.
