Aluminium-26 from Massive Binary Stars. I. Nonrotating Models
Aluminium-26 from Massive Binary Stars. I. Nonrotating Models
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DOI：
10.3847/1538-4357/ab40ae
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发表时间：
2019-09
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影响因子：
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通讯作者：
H. Brinkman;Carolyn Doherty;O. Pols;Er-Tao Li;B. Cot'e;M. Lugaro
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作者：
H. Brinkman;Carolyn Doherty;O. Pols;Er-Tao Li;B. Cot'e;M. Lugaro
铝-26是一种半衰期为72万年的短寿命放射性核素，目前在银河系中通过γ射线光谱法观测到，并通过对陨石的分析推断其存在于早期太阳系中。大质量恒星被认为是26Al的主要贡献者。虽然大多数大质量恒星都是在双星系统中发现的，但是自从Braun & Langer以来，双星相互作用对26 Al产额的影响还没有被研究过。我们的目标是填补这一空白。我们用MESA恒星演化程序计算了大质量（10 M <$≤ M ≤ 80 M <$）太阳金属丰度（Z = 0.014）的非旋转单星和双星。我们计算的风产量的单星和双星系统的质量转移起着重要作用。根据主星星的初始质量和轨道周期，26 Al产额在双星系统中可以增加或减少。对于一次质量在1.35 - 40 M <$A的双星系统，产额可以显著增加，特别是在较低质量端，而在1.45 M <$A以上，产额变得与单星产额相似，甚至下降。我们的初步结果表明，相比超新星爆炸，质量损失的贡献在二进制系统的总26铝丰度产生的恒星人口是次要的。另一方面，如果大质量星星质量损失是早期太阳系中26 Al的起源，那么我们的结果将对潜在恒星或恒星群来源的识别产生重大影响。
Aluminium-26 is a short-lived radionuclide with a half-life of 0.72 Myr, which is observed today in the Galaxy via γ-ray spectroscopy and is inferred to have been present in the early solar system via analysis of meteorites. Massive stars are considered the main contributors of 26Al. Although most massive stars are found in binary systems, the effect, however, of binary interactions on the 26Al yields has not been investigated since Braun & Langer. Here we aim to fill this gap. We have used the MESA stellar evolution code to compute massive (10 M⊙ ≤ M ≤ 80 M⊙) nonrotating single and binary stars of solar metallicity (Z = 0.014). We computed the wind yields for the single stars and for the binary systems where mass transfer plays a major role. Depending on the initial mass of the primary star and orbital period, the 26Al yield can either increase or decrease in a binary system. For binary systems with primary masses up to ∼35–40 M⊙, the yield can increase significantly, especially at the lower mass end, while above ∼45 M⊙ the yield becomes similar to the single-star yield or even decreases. Our preliminary results show that compared to supernova explosions, the contribution of mass loss in binary systems to the total 26Al abundance produced by a stellar population is minor. On the other hand, if massive star mass loss is the origin of 26Al in the early solar system, our results will have significant implications for the identification of the potential stellar, or stellar population, source.