大质量恒星的命运：用METISSE探索恒星演化中的不确定性
The fates of massive stars: exploring uncertainties in stellar evolution with METISSE
摘要：
在先进的电磁波和引力波探测器时代，有效结合和研究恒星演化对双星和恒星动力学系统的影响变得越来越重要。系统的研究致力于探索恒星演化中的不确定参数，以解释最近对恒星星族的观测。我们提出了一种新的方法，常用的单星进化（SSE）拟合公式，一个更适应：单星进化插值方法（METISSE）。它利用预先计算的恒星轨道集之间的插值来近似恒星种群的演化参数。我们已经使用METISSE与详细的恒星轨道计算的恒星天体物理学实验模块（MESA），波恩进化代码（BEC）和剑桥星代码。与SSE相比，METISSE更好地再现了使用STARS代码计算的恒星轨迹，并且平均快三倍。使用MESA和BEC计算的恒星轨迹，我们应用METISSE探索大质量恒星的残余质量，最大径向膨胀和主序星寿命的差异。我们发现，恒星演化中使用的不同物理成分，例如辐射主导的包络的处理，可以影响它们的演化结果。对于质量范围在9到100 M $_\odot$的恒星，残余质量的预测可以相差20 M $_\odot$，而恒星所达到的最大径向膨胀在不同的恒星模型之间可以相差一个数量级。
英文摘要：
In the era of advanced electromagnetic and gravitational wave detectors, it has become increasingly important to effectively combine and study the impact of stellar evolution on binaries and dynamical systems of stars. Systematic studies dedicated to exploring uncertain parameters in stellar evolution are required to account for the recent observations of the stellar populations. We present a new approach to the commonly used Single-Star Evolution (SSE) fitting formulae, one that is more adaptable: Method of Interpolation for Single Star Evolution (METISSE). It makes use of interpolation between sets of pre-computed stellar tracks to approximate evolution parameters for a population of stars. We have used METISSE with detailed stellar tracks computed by the Modules for Experiments in Stellar Astrophysics (MESA), Bonn Evolutionary Code (BEC) and Cambridge STARS code. METISSE better reproduces stellar tracks computed using the STARS code compared to SSE, and is on average three times faster. Using stellar tracks computed with MESA and BEC, we apply METISSE to explore the differences in the remnant masses, the maximum radial expansion, and the main-sequence lifetime of massive stars. We find that different physical ingredients used in the evolution of stars, such as the treatment of radiation dominated envelopes, can impact their evolutionary outcome. For stars in the mass range 9 to 100 M$_\odot$, the predictions of remnant masses can vary by up to 20 M$_\odot$, while the maximum radial expansion achieved by a star can differ by an order of magnitude between different stellar models.
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