论文标题
非常巨大的恒星作为短寿命放射性同位素的来源$^{26} $ al
Very massive star winds as sources of the short-lived radioactive isotope $^{26}$Al
论文作者
论文摘要
$^{26} $短寿命的放射性核素是观察到的银河弥漫性$γ$ -RARE发射1.8 meV的来源。虽然已经探索了$^{26} $ al的不同来源，例如AGB恒星，巨大的恒星风和超新星，但从未研究过非常巨大的恒星的贡献。我们研究了非常巨大的恒星的恒星风贡献，即，在$^{26} $ al的富集中，恒星的初始质量在150至300 m $ _ \ odot $之间。我们通过研究旋转和非旋转非常巨大的恒星模型，讨论$^{26} $ al的生产，其初始质量在150至300 m $ $ _ \ odot $之间，金属金属Z = 0.006、0.014和0.020。我们将这一结果面对一个简单的银河系模型，同时考虑了金属性和恒星形成速率梯度。我们获得了Z = 0.006-0.020金属度范围中的非常大的恒星可能是$^{26} $ all富集星际介质的重要贡献者。通常，当考虑到非常巨大的恒星时，大恒星的风对银河系中$^{26} $ al的总数的贡献会增加150 \％。尽管很少见，但非常庞大的恒星可能是$^{26} $ al的重要贡献者，总体上非常重要的参与者是银河系中的核合成。
The $^{26}$Al short-lived radioactive nuclide is the source of the observed galactic diffuse $γ$-ray emission at 1.8 MeV. While different sources of $^{26}$Al have been explored, such as AGB stars, massive stars winds, and supernovae, the contribution of very massive stars has never been studied. We study the stellar wind contribution of very massive stars, i.e stars with initial masses between 150 and 300 M$_\odot$, to the enrichment in $^{26}$Al of the galactic interstellar medium. We discuss the production of $^{26}$Al by studying rotating and non-rotating very massive stellar models with initial masses between 150 and 300 M$_\odot$ for metallicities Z=0.006, 0.014, and 0.020. We confront this result to a simple Milky Way model taking into account both the metallicity and the star formation rate gradients. We obtain that very massive stars in the Z=0.006-0.020 metallicity range might be very significant contributors to the $^{26}$Al enrichment of the interstellar medium. Typically, the contribution of the winds of massive stars to the total quantity of $^{26}$Al in the Galaxy increases by 150\% when very massive stars are considered. Very massive stars, despite their rarity, might be important contributors to $^{26}$Al and overall very important actors for nucleosynthesis in the Galaxy.
