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arXiv 1809.01673astro-ph.SR
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0.85 - 7.5 M的白矮星初终质量关系（$_\odot$）

The White Dwarf Initial-Final Mass Relation for Progenitor Stars From 0.85 to 7.5 M$_\odot$

Jeffrey D. Cummings, Jason S. Kalirai, P. -E. Tremblay, Enrico Ramirez-Ruiz, Jieun Choi

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14 pages, 6 figures, accepted for publication in ApJ
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摘要：

通过对天狼星B和来自13个星团的79颗白矮星的自洽分析，给出了它们的初末质量关系。我们还获得了先前在NGC 2099星团场中分析过的八颗白矮星的额外信号，其中四颗与成员一致。这些重新观测到的白矮星的质量范围从0.72到0.97 M $_\odot$，初始质量从3.0到3.65 M $_\odot$，IFMR在斜率上有一个重要的变化，这些新的数据有助于观测证实。总的来说，该直接测量的IFMR具有小的散射（$σ$ = 0.06 M $_\odot$），并且从0.85至7.5 M $_\odot$的祖细胞跨越。应用两种不同的恒星演化模型来推断两组不同的白矮星祖先质量表明，当同样的模型也被用来推导星系团的年龄，所得到的IFMR有弱的敏感性，通过模型，但在所有最高的初始质量（$>$ 5.5 M $_\odot$）。还清楚地观察到IFMR的非线性，在较低质量（0.08 M $_{\rm final}$ /M $_{\rm initial}$）和较高质量（0.11 M $_{\rm final}$ /M $_{\rm initial}$）下具有中等斜率，其被2.85至3.6 M $_\odot$的祖细胞之间的陡峭斜率（0.19 M $_{\rm final}$ /M $_{\rm initial}$）分解。该IFMR显示，恒星总质量损失范围从0.83 M $_\odot$时的M $_{\rm initial}$的33%到7.5 M $_\odot$时的M $_{\rm initial}$的83%。然而，测试这种总质量损失对祖金属丰度的依赖性，发现在-0.15 $<$ [Fe/H] $<$ +0.15的中等范围内没有可检测的灵敏度。

英文摘要：

We present the initial-final mass relation (IFMR) based on the self-consistent analysis of Sirius B and 79 white dwarfs from 13 star clusters. We have also acquired additional signal on eight white dwarfs previously analyzed in the NGC 2099 cluster field, four of which are consistent with membership. These reobserved white dwarfs have masses ranging from 0.72 to 0.97 M$_\odot$, with initial masses from 3.0 to 3.65 M$_\odot$, where the IFMR has an important change in slope that these new data help to observationally confirm. In total, this directly measured IFMR has small scatter ($σ$ = 0.06 M$_\odot$) and spans from progenitors of 0.85 to 7.5 M$_\odot$. Applying two different stellar evolutionary models to infer two different sets of white dwarf progenitor masses shows that when the same model is also used to derive the cluster ages, the resulting IFMR has weak sensitivity to the adopted model at all but the highest initial masses ($>$5.5 M$_\odot$). The non-linearity of the IFMR is also clearly observed with moderate slopes at lower masses (0.08 M$_{\rm final}$/M$_{\rm initial}$) and higher masses (0.11 M$_{\rm final}$/M$_{\rm initial}$) that are broken up by a steep slope (0.19 M$_{\rm final}$/M$_{\rm initial}$) between progenitors from 2.85 to 3.6 M$_\odot$. This IFMR shows total stellar mass loss ranges from 33\% of M$_{\rm initial}$ at 0.83 M$_\odot$ to 83\% of M$_{\rm initial}$ at 7.5 M$_\odot$. Testing this total mass loss for dependence on progenitor metallicity, however, finds no detectable sensitivity across the moderate range of -0.15 $<$ [Fe/H] $<$ +0.15.

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