早期宇宙中3000 M$_\odot$恒星的演化与影响
The evolution and impact of 3000 M$_\odot$ stars in the early Universe
AI总结：
本文提出了早期宇宙中大质量吸积population III恒星的演化模型，探讨了3000 Msol恒星在硅燃烧结束前的演化特征及其对周围环境化学演化和反馈的潜在影响。
摘要：
我们提出了大质量吸积population III（第三星族）恒星的演化模型，采用恒定和可变吸积率直到硅燃烧结束，最终质量为1000 - 3000 Msol。在我们所有的模型中，核心氢燃烧阶段之后，恒星向Hertzsprung-Russell图的红侧膨胀，并在此度过其余演化过程。在核心氦燃烧期间，模型表现出外部对流包层以及许多大型中间对流区。这些中间区域允许发生强烈的内部混合，使表面氦丰度增加。在10^{-3} Msol/yr的恒定吸积率下，金属丰度增加的效应显示寿命、最终质量和包层中氦的分布均有所增加。我们的基准模型质量为3000 Msol，其最终表面氦丰度为0.74，且总质量的9%或核心质量的50%在核心硅燃烧结束时具有Gamma1 < 4/3的值。如果核心坍缩伴随着碳氧核心外部的包层抛射，这可能对周围环境的化学演化及后续恒星世代产生重大影响。该模型最终的log(N/O) ~ 0.45，高于最近探测到的高红移星系GN-z11的下限。我们讨论了单个3000 Msol恒星对化学、力学和辐射反馈的影响，并提出了未来工作的方向。
英文摘要：
We present evolutionary models of massive, accreting population III stars with constant and variable accretion rates until the end of silicon burning, with final masses of 1000 - 3000 Msol. In all our models, after the core-hydrogen-burning phase, the star expands towards the red side of the Hertzsprung-Russell diagram is where it spends the rest of its evolution. During core helium burning, the models exhibit an outer convective envelope as well as many large intermediate convective zones.These intermediate zones allow for strong internal mixing to occur which enriches the surface in helium. The effect of increasing metallicity at a constant accretion rate of 10^{-3} Msol/yr shows an increase in the lifetime, final mass and distribution of helium in the envelope. Our fiducial model with mass of 3000 Msol has a final surface helium abundance of 0.74 and 9% of its total mass or 50% of the core mass, has a value of Gamma1 < 4/3 at the end of core silicon burning. If the collapse of the core is accompanied by the ejection of the envelope above the carbon-oxygen core, this could have a significant impact on the chemical evolution of the surroundings and subsequent stellar generations. The model has a final log(N/O) ~ 0.45, above the lower limit in the recently detected high-redshift galaxy GN-z11. We discuss the impact of a single 3000 Msol star on chemical, mechanical and radiative feedback, and present directions for future work.
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