氦巨星作为快速衰落的Ibc型超新星的祖先
Helium giant stars as progenitors of rapidly fading Type Ibc supernovae
摘要：
I型快速衰落超新星（RFSNe）似乎起源于无氢恒星，具有大半径，产生主要是冲击冷却的光变曲线，与更典型的富镍SNe Ibc形成对比。然而，仍然需要确定哪些类型的恒星会产生明亮的冲击冷却光变曲线，而没有放射性镍的显着贡献。质量在2-4个太阳质量范围内的裸氦星，由于核心外的氦和碳壳层燃烧强烈，密度梯度很大，因此已知流体静力学发展的半径可达100个太阳半径或更大。我们制作了几个这样的恒星模型，并证明，当爆炸时，这些氦巨星可以自然地产生RFSN光变曲线。由于许多原型SNe Ibc也应该来自这个质量范围内的大半径恒星，我们预测这些RFSNe可能与SNe Ibc不同，这仅仅是因为没有大量的镍。
英文摘要：
Type I rapidly fading supernovae (RFSNe) appear to originate from hydrogen-free stars with large radii that produce predominantly shock-cooling light curves, in contrast with more typical nickel-rich SNe Ibc. However, it remains to be determined what types of stars would produce bright shock-cooling light curves without significant contribution from radioactive nickel. Bare helium stars in the mass range ~2-4 solar masses are known to hydrostatically develop radii as large as 100 solar radii or more due to strong He and C shell burning outside of a core with a sharp density gradient. We produce several such stellar models and demonstrate that, when exploded, these helium giants can naturally produce RFSN light curves. Since many prototypical SNe Ibc should come from large-radius stars in this mass range as well, we predict that these RFSNe may be distinct from SNe Ibc solely due to the absence of substantial nickel.
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