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Title: MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA): PLANETS, OSCILLATIONS, ROTATION, AND MASSIVE STARS

We substantially update the capabilities of the open source software package Modules for Experiments in Stellar Astrophysics (MESA), and its one-dimensional stellar evolution module, MESA star. Improvements in MESA star's ability to model the evolution of giant planets now extends its applicability down to masses as low as one-tenth that of Jupiter. The dramatic improvement in asteroseismology enabled by the space-based Kepler and CoRoT missions motivates our full coupling of the ADIPLS adiabatic pulsation code with MESA star. This also motivates a numerical recasting of the Ledoux criterion that is more easily implemented when many nuclei are present at non-negligible abundances. This impacts the way in which MESA star calculates semi-convective and thermohaline mixing. We exhibit the evolution of 3-8 M{sub Sun} stars through the end of core He burning, the onset of He thermal pulses, and arrival on the white dwarf cooling sequence. We implement diffusion of angular momentum and chemical abundances that enable calculations of rotating-star models, which we compare thoroughly with earlier work. We introduce a new treatment of radiation-dominated envelopes that allows the uninterrupted evolution of massive stars to core collapse. This enables the generation of new sets of supernovae, long gamma-ray burst, and pair-instability progenitormore » models. We substantially modify the way in which MESA star solves the fully coupled stellar structure and composition equations, and we show how this has improved the scaling of MESA's calculational speed on multi-core processors. Updates to the modules for equation of state, opacity, nuclear reaction rates, and atmospheric boundary conditions are also provided. We describe the MESA Software Development Kit that packages all the required components needed to form a unified, maintained, and well-validated build environment for MESA. We also highlight a few tools developed by the community for rapid visualization of MESA star results.« less
Authors:
; ;  [1] ;  [2] ;  [3] ;  [4] ;  [5] ;  [6] ;  [7] ;  [8] ;  [9]
  1. Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106 (United States)
  2. Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904-4325 (United States)
  3. Department of Physics and Astronomy, National Superconducting Cyclotron Laboratory, and Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, MI 48864 (United States)
  4. Research School of Astronomy and Astrophysics, The Australian National University, Weston, ACT 2611 (Australia)
  5. Department of Physics, University of California, Santa Barbara, CA 93106 (United States)
  6. Department of Astronomy and McDonald Observatory, University of Texas, Austin, TX 78712 (United States)
  7. Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006 (Australia)
  8. School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287 (United States)
  9. Department of Astronomy, University of Wisconsin-Madison, Madison, WI 53706 (United States)
Publication Date:
OSTI Identifier:
22136508
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal, Supplement Series; Journal Volume: 208; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ABUNDANCE; ANGULAR MOMENTUM; BOUNDARY CONDITIONS; COMPUTER CODES; COOLING; COSMIC GAMMA BURSTS; EQUATIONS OF STATE; HELIUM BURNING; NUCLEAR REACTIONS; NUCLEI; ONE-DIMENSIONAL CALCULATIONS; OPACITY; OSCILLATIONS; PULSATIONS; REACTION KINETICS; ROTATION; SCALING; STAR EVOLUTION; STAR MODELS; SUPERNOVAE; WHITE DWARF STARS