自转大质量恒星的前超新星演化和爆炸性核合成。II.Fe/H] = 0.3 时的超太阳模型

Lorenzo Roberti, Marco Limongi and Alessandro Chieffi
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摘要

我们介绍了Limongi & Chieffi(2018)发表的一组模型在2倍太阳金属性(即[Fe/H] = 0.3)下的扩展。这些模型在内核坍缩开始时的关键物理特性主要是由于较高的金属性引发了较高的质量损失:超太阳金属性(SSM)模型以较小的 He 和 CO 内核质量达到内核坍缩,而中心 He 燃烧留下的 12C 量较高。这些结果适用于所有旋转速度。在非旋转情况下,以单位质量氧(即 X/O)表示的中子俘获核的产率在 SSM 模型中高于 SM 模型,而在旋转模型中则相反。考虑到中子俘获核合成的次级性质,非旋转模型所显示的趋势是意料之中的。反之亦然,旋转模型中出现的反直觉趋势是 SSM 模型中质量损失较大的结果,当恒星仍处于中心氦燃烧时,SSM 模型比 SM 模型更快地移除富含 H 的包层,甩掉纠缠(由旋转不稳定性激活),从而甩掉明显的初级中子捕获核合成。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Presupernova Evolution and Explosive Nucleosynthesis of Rotating Massive Stars. II. The Supersolar Models at [Fe/H] = 0.3
We present an extension of the set of models published in Limongi & Chieffi (2018) at metallicity 2 times solar, i.e., [Fe/H] = 0.3. The key physical properties of these models at the onset of core collapse are mainly due to the higher mass loss triggered by the higher metallicity: the supersolar metallicity (SSM) models reach core collapse with smaller He- and CO-core masses, while the amount of 12C left by the central He burning is higher. These results are valid for all the rotation velocities. The yields of the neutron-capture nuclei expressed per unit mass of oxygen (i.e., the X/O) are higher in the SSM models than in the SM ones in the nonrotating case, while the opposite occurs in the rotating models. The trend shown by the nonrotating models is the expected one, given the secondary nature of the neutron-capture nucleosynthesis. Vice versa, the counterintuitive trend obtained in the rotating models is the consequence of the higher mass loss present in the SSM models, removes the H-rich envelope faster than in the SM models while the stars are still in central He burning, dumping out the entanglement (activated by the rotation instabilities) and therefore conspicuous primary neutron-capture nucleosynthesis.
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