MESA (Modules for Experiments in Stellar Astrophysics )

Открытые коды для расчета звездной эволюции и строения звезд. Созданы международной группой астрофизиков.

Основная статья: Modules for Experiments in Stellar Astrophysics pdf файл статьи
Author
Bill Paxton¹, Lars Bildsten¹, Aaron Dotter^2,5, Falk Herwig², Pierre Lesaffre³ and Frank Timmes⁴
Affiliations
1 Kavli Institute for Theoretical Physics and Department of Physics, Kohn Hall, University of California, Santa Barbara, CA 93106, USA
2 Department of Physics and Astronomy, University of Victoria, P.O. Box 3055, STN CSC, Victoria, BC V8W 3P6, Canada
3 LERMA-LRA, CNRS UMR8112, Observatoire de Paris and Ecole Normale Superieure, 24 Rue Lhomond, 75231 Paris Cedex 05, France
4 School of Earth and Space Exploration, Arizona State University, P.O. Box 871404, Tempe, AZ 85287-1404, USA
5 Current address: Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA.
Journal
The Astrophysical Journal Supplement Series Create an alert RSS this journal
Issue
Volume 192, Number 1
Citation
Bill Paxton et al. 2011 ApJS 192 3
doi: 10.1088/0067-0049/192/1/3
Abstract

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/).