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arXiv 2303.05083astro-ph.SRastro-ph.HE
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氧-氖和碳-氧白矮星对合并后残余物的演化

Evolution of the post merger remnants from the coalescence of oxygen-neon and carbon-oxygen white dwarf pairs

Chengyuan Wu, Heran Xiong, Jie Lin, Yunlang Guo, Xiaofeng Wang, Zhanwen Han, Bo Wang

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22 pages, 10 figures, 8 tables, accepted for publication in ApJL
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摘要：

虽然多维模拟研究了双WD合并的过程，合并后的演变只集中在碳氧（CO）WD或氦（He）WD合并残留物。在这项工作中，我们调查的第一次演变的残余物源于合并的氧氖（ONe）WD与CO WD。我们的模拟结果表明，合并残留物可以演变成氢和氦缺乏巨星，最大半径约为300 Rsun。我们的模型表明，合并残留物质量超过1.95 Msun可以点燃Ne之前显着的质量损失enclaimer，因此，他们将成为电子捕获超新星（ECSNe）。然而，初始质量小于1.90Msun的残留物将经历进一步的核心收缩和更长的演化时间，才达到Ne燃烧的条件。因此，它们的命运更依赖于恒星风造成的质量损失率，因此更不确定。相对较高的质量损失率将导致这些残留物以一个WD结束其生命。我们的演化模型可以很自然地解释双WD合并残留IRAS 00500+6713（J 005311）的观测特性。如文献中先前所述，我们提出并证明J 005311可能是ONe WD和CO WD合并的残留物。我们推断，J 005311的最终结果将是一个巨大的ONe WD，而不是超新星爆炸。我们的调查可能能够提供可能的限制风的质量损失性质的巨人有CO占主导地位的信封。

英文摘要：

Although multidimensional simulations have investigated the processes of double WD mergers, post-merger evolution only focused on the carbon-oxygen (CO) WD or helium (He) WD merger remnants. In this work, we investigate for the first time the evolution of the remnants stemmed from the merger of oxygen-neon (ONe) WDs with CO WDs. Our simulation results indicate that the merger remnants can evolve to hydrogen- and helium-deficient giants with maximum radius of about 300Rsun. Our models show evidence that merger remnants more massive than 1.95Msun can ignite Ne before significant mass-loss ensues, and they thus would become electron-capture supernovae (ECSNe). However, remnants with initial masses less than 1.90Msun will experience further core contraction and longer evolutionary time before reaching at the conditions for Ne-burning. Therefore their fates are more dependent on mass-loss rates due to stellar winds, and thus more uncertain. Relatively high mass-loss rates would cause such remnants to end their lives as ONe WDs. Our evolutionary models can naturally explain the observational properties of the double WD merger remnant IRAS 00500+6713 (J005311). As previously suggested in the literature, we propose and justify that J005311 may be the remnant from the coalescence of an ONe WD and an CO WD. We deduce that the final outcome of J005311 would be a massive ONe WD rather than a supernova explosion. Our investigations may be able to provide possible constraints on the wind mass-loss properties of the giants which have CO-dominant envelopes.

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