arXiv 2001.087112020-01-23astro-ph.SRastro-ph.GA

核坍缩超新星和直接坍缩黑洞的不确定质量

The Uncertain Masses of Progenitors of Core Collapse Supernovae and Direct Collapse Black Holes

Eoin Farrell, Jose Groh, Georges Meynet, JJ Eldridge

备注：: Re-submitted to MNRAS Letters after referee comments
DOI：: 10.1093/mnrasl/slaa035

摘要：

我们指出，仅仅从红超巨星的光度$L$和有效温度$T_{\rm eff}$是不可能确定红超巨星在前超新星阶段的最终质量$M_{\rm fin}$的。使用恒星模型的网格，我们证明，对于一个给定的$L$和$T_{\rm eff}$值，RSG可以有一个范围为3至$45~\mathrm{M}_{\odot}$的$M_{\rm fin}$。虽然这些限值内的概率分布不是平坦的，但RSG的任何$M_{\rm fin}$的单独测定都将是退化的。这使得难以确定其进化历史并将$M_{\rm fin}$映射到初始质量。单颗恒星产生的范围较窄，如果不对质量损失、对流和旋转做出强有力的假设，就很难准确确定。二进制将产生更广泛的RSG $M_{\rm fin}$。然而，最终的氦核质量M $_{\rm He-core}$是由最终的光度确定的，我们发现$\log (\mathrm{M}_{\rm He-core}/M_{\odot}) = 0.659 \log (L/\mathrm{L}_{\odot}) -2.630$使用这种关系，我们推导出直接成像的SN祖先和一个失败的SN候选者的M $_{\rm He-core}$。由于$T_{\rm eff}$依赖于$M_{\rm env} \lesssim 1~$ M $_{\odot}$的包络质量$M_{\rm env}$，所以SNe IIb的剥离恒星祖先的$M_{\rm fin}$值更好地受到$L$和$T_{\rm eff}$的约束。在给定初始质量函数的情况下，我们的结果适用于大多数核坍缩黑洞、失败黑洞和直接坍缩黑洞的祖先。

英文摘要：

We show that it is not possible to determine the final mass $M_{\rm fin}$ of a red supergiant (RSG) at the pre-supernova (SN) stage from its luminosity $L$ and effective temperature $T_{\rm eff}$ alone. Using a grid of stellar models, we demonstrate that for a given value of $L$ and $T_{\rm eff}$, a RSG can have a range of $M_{\rm fin}$ as wide as 3 to $45~\mathrm{M}_{\odot}$. While the probability distribution within these limits is not flat, any individual determination of $M_{\rm fin}$ for a RSG will be degenerate. This makes it difficult to determine its evolutionary history and to map $M_{\rm fin}$ to an initial mass. Single stars produce a narrower range that is difficult to accurately determine without making strong assumptions about mass loss, convection, and rotation. Binaries would produce a wider range of RSG $M_{\rm fin}$. However, the final Helium core mass M$_{\rm He-core}$ is well determined by the final luminosity and we find $\log (\mathrm{M}_{\rm He-core}/M_{\odot}) = 0.659 \log (L/\mathrm{L}_{\odot}) -2.630$ Using this relationship, we derive M$_{\rm He-core}$ for directly imaged SN progenitors and one failed SN candidate. The value of $M_{\rm fin}$ for stripped star progenitors of SNe IIb is better constrained by $L$ and $T_{\rm eff}$ due to the dependence of $T_{\rm eff}$ on the envelope mass $M_{\rm env}$ for $M_{\rm env} \lesssim 1~$M$_{\odot}$. Given the initial mass function, our results apply to the majority of progenitors of core collapse SNe, failed SNe and direct collapse black holes.

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