MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA): BINARIES, PULSATIONS, AND EXPLOSIONS
MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA): BINARIES, PULSATIONS, AND EXPLOSIONS
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DOI：
10.1088/0067-0049/220/1/15
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发表时间：
2015-06
期刊：
影响因子：
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通讯作者：
B. Paxton;P. Marchant;J. Schwab;E. Bauer;L. Bildsten;L. Bildsten;M. Cantiello;L. Dessart;
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文献类型：
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作者：
B. Paxton;P. Marchant;J. Schwab;E. Bauer;L. Bildsten;L. Bildsten;M. Cantiello;L. Dessart;
我们实质性地更新了开源软件仪器模块在恒星天体物理实验（MESA）的功能。MESA现在可以同时演化一对相互作用的差转恒星，经历质量和角动量的转移和损失，大大增强了先前模拟双星演化的能力。MESA在核网络与数百种同位素的完全耦合计算方面的新能力现在允许MESA精确模拟构建超新星祖模型所需的高级燃烧阶段。带有激波的隐式流体动力学现在可以用MESA进行处理，从而可以对整个大质量恒星的生命周期进行建模，从主序前的演化到核心坍缩的开始，以及由此产生的爆炸的核合成。GYRE非绝热脉动仪与MESA的耦合允许对大质量恒星的不稳定带进行新的探索，同时也加速了天体物理学对星震学数据的使用。我们改进了质量吸积的处理，提供了更准确和稳健的近地表剖面。MESA可以根据输入的核数据“动态”计算弱反应速率，从而更好地模拟大质量白矮星的吸积坍缩和一些大质量恒星的命运。我们讨论了在强耦合等离子体状态下化学扩散的持续挑战，并展示了MESA的改进，现在允许模拟热恒星中重元素的辐射悬浮。最后，我们注意到MESA软件基础设施在所有支持的平台上为所有结果提供了位对位的一致性，这是加速MESA发展的深刻支持能力。
We substantially update the capabilities of the open-source software instrument Modules for Experiments in Stellar Astrophysics (MESA). MESA can now simultaneously evolve an interacting pair of differentially rotating stars undergoing transfer and loss of mass and angular momentum, greatly enhancing the prior ability to model binary evolution. New MESA capabilities in fully coupled calculation of nuclear networks with hundreds of isotopes now allow MESA to accurately simulate the advanced burning stages needed to construct supernova progenitor models. Implicit hydrodynamics with shocks can now be treated with MESA, enabling modeling of the entire massive star lifecycle, from pre-main-sequence evolution to the onset of core collapse and nucleosynthesis from the resulting explosion. Coupling of the GYRE non-adiabatic pulsation instrument with MESA allows for new explorations of the instability strips for massive stars while also accelerating the astrophysical use of asteroseismology data. We improve the treatment of mass accretion, giving more accurate and robust near-surface profiles. A new MESA capability to calculate weak reaction rates “on-the-fly” from input nuclear data allows better simulation of accretion induced collapse of massive white dwarfs and the fate of some massive stars. We discuss the ongoing challenge of chemical diffusion in the strongly coupled plasma regime, and exhibit improvements in MESA that now allow for the simulation of radiative levitation of heavy elements in hot stars. We close by noting that the MESA software infrastructure provides bit-for-bit consistency for all results across all the supported platforms, a profound enabling capability for accelerating MESA's development.