论文标题
具有台面的太阳能恒星中的原子扩散。与蒙特利尔/蒙彼利埃和Cestam Stellar Evolution代码进行比较
Atomic diffusion in solar-like stars with MESA. Comparison with the Montreal/Montpellier and CESTAM stellar evolution codes
论文作者
论文摘要
恒星天体物理学实验（MESA）实验的恒星进化代码模块是公开的，并且被社区广泛使用。它包括考虑几个非标准过程，例如原子扩散。即使重力沉降的效果被认为是当今恒星建模中的标准成分，辐射加速度并非如此。原子扩散以及辐射加速度的特定处理从未与其他恒星进化代码进行比较。为这些代码进行基准测试很重要，因为为了分析当前和未来空间任务的数据，例如\ textit {kepler}，过境外球形调查卫星（TESS）以及星球传输和恒星（柏拉图）任务的振荡。 本文的目的是将包括原子扩散（辐射加速度）在内的MESA模型与使用蒙特利尔/蒙彼利埃恒星恒星进化代码计算的模型以及代码d'Evolution Stellaire adaptatif et Modulaire（Cestam）进行比较。此外，我们评估了与原子扩散有关的某些台面选项的影响。 我们根据14个元素具有台化模型的丰度，计算了原子扩散，包括辐射加速度。然后将其与使用Montreal/Montpellier和Cestam代码计算的1.1和1.1和1.1和1.4〜 $ M _ {\ odot} $模型进行了比较。还通过一次只改变其中一个测试，用于原子扩散的各种测试。 我们发现，当仔细设置原子扩散选项时，台面模型中考虑元素的丰度曲线与使用其他两个代码计算的模型进行了很好的比较。我们还表明，MESA中的某些选择对于正确治疗原子扩散至关重要。
The stellar evolution code Modules for Experiments in Stellar Astrophysics (MESA) is public and is widely used by the community. It includes the possibility of taking several non-standard processes such as atomic diffusion into account. Even if the effect of gravitational settling is considered a standard ingredient in stellar modelling today, this is not the case for radiative accelerations. The specific treatment of atomic diffusion along with the radiative accelerations has never been compared with other stellar evolution codes. Benchmarking these codes is important because improved accuracy is required in order to analyse data from present and future space missions, such as the \textit{Kepler}, Transiting Exoplanet Survey Satellite (TESS), and PLAnetary Transits and Oscillations of stars (PLATO) missions. The aim of this paper is to compare MESA models including atomic diffusion (with radiative accelerations) with models computed with the Montreal/Montpellier stellar evolution code and with the Code d'Evolution Stellaire Adaptatif et Modulaire (CESTAM). Additionally, we assess the impact of some MESA options related to atomic diffusion. We calculated atomic diffusion, including radiative accelerations, following the abundance profiles of 14 elements with MESA models. This was then compared with 1.1 and 1.4~$M_{\odot}$ models computed with the Montreal/Montpellier and CESTAM codes. Various tests of MESA options for atomic diffusion were also carried out by varying only one of them at a time. We find that the abundance profiles of the considered elements in the MESA models compare rather well with the models computed with the two other codes when atomic diffusion options are carefully set. We also show that some options in MESA are crucial for a proper treatment of atomic diffusion.
