MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA)
MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA)
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DOI：
10.1088/0067-0049/192/1/3
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发表时间：
2010-09
期刊：
影响因子：
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通讯作者：
B. Paxton;L. Bildsten;A. Dotter;F. Herwig;P. Lesaffre;F. Timmes
中科院分区：
文献类型：
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作者：
B. Paxton;L. Bildsten;A. Dotter;F. Herwig;P. Lesaffre;F. Timmes
恒星物理学和演化计算使天体物理学的研究范围更广。恒星天体物理实验模块(MESA)是一套开源、健壮、高效、线程安全的库，适用于计算恒星天体物理中的广泛应用。一维恒星演化模块MESAstar结合了许多数值和物理模块，用于模拟从极低质量到大质量恒星的各种恒星演化场景，包括高级演化阶段。MESAstar同时求解完全耦合的结构方程和组成方程。它使用自适应网格细化和复杂的时间步长控制，并支持基于OpenMP的共享内存并行。最先进的模块提供状态方程、不透明度、核反应速率、元素扩散数据和大气边界条件。每个模块都被构建为一个单独的Fortran 95库，该库具有自己明确定义的公共接口，以促进独立开发。几个详细的例子表明了持续进行的广泛的核查和测试，并展示了MESA拥有的广泛能力。这些例子包括：极低质量恒星、棕矮星和气态巨行星到非常老年龄的演化轨迹；1 M☉恒星从前主序列到冷却白矮星的完整演化轨迹；太阳声速分布；中等质量恒星通过氦核心燃烧阶段和氦壳层燃烧渐近巨型分支阶段的热脉冲演化；缓慢脉动的B星和贝塔造父变星的内部结构；大质量恒星从主序前到核心塌缩开始的完整演化轨迹；经历罗氏叶溢出的恒星的质量转移；氦吸积向中子星的演化。MESA可从项目网站(http://mesa.sourceforge.net/).)下载
Stellar physics and evolution calculations enable a broad range of research in astrophysics. Modules for Experiments in Stellar Astrophysics (MESA) is a suite of open source, robust, efficient, thread-safe libraries for a wide range of applications in computational stellar astrophysics. A one-dimensional stellar evolution module, MESAstar, combines many of the numerical and physics modules for simulations of a wide range of stellar evolution scenarios ranging from very low mass to massive stars, including advanced evolutionary phases. MESAstar solves the fully coupled structure and composition equations simultaneously. It uses adaptive mesh refinement and sophisticated timestep controls, and supports shared memory parallelism based on OpenMP. State-of-the-art modules provide equation of state, opacity, nuclear reaction rates, element diffusion data, and atmosphere boundary conditions. Each module is constructed as a separate Fortran 95 library with its own explicitly defined public interface to facilitate independent development. Several detailed examples indicate the extensive verification and testing that is continuously performed and demonstrate the wide range of capabilities that MESA possesses. These examples include evolutionary tracks of very low mass stars, brown dwarfs, and gas giant planets to very old ages; the complete evolutionary track of a 1 M☉ star from the pre-main sequence (PMS) to a cooling white dwarf; the solar sound speed profile; the evolution of intermediate-mass stars through the He-core burning phase and thermal pulses on the He-shell burning asymptotic giant branch phase; the interior structure of slowly pulsating B Stars and Beta Cepheids; the complete evolutionary tracks of massive stars from the PMS to the onset of core collapse; mass transfer from stars undergoing Roche lobe overflow; and the evolution of helium accretion onto a neutron star. MESA can be downloaded from the project Web site (http://mesa.sourceforge.net/).