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Jermyn, Adam S.; Bauer, Evan B.; Schwab, Josiah; Farmer, R.; Ball, Warrick H.; Bellinger, Earl P.; Dotter, Aaron; Joyce, Meridith; Marchant, Pablo; Mombarg, Joey S. G.; Wolf, William M.; Sunny Wong, Tin Long; Cinquegrana, Giulia C.; Farrell, Eoin; Smolec, R.; Thoul, Anne; Cantiello, Matteo; Herwig, Falk; Toloza, Odette; Bildsten, Lars; Townsend, Richard H. D.; Timmes, F. X.

Modules for Experiments in Stellar Astrophysics (MESA): Time-dependent Convection, Energy Conservation, Automatic Differentiation, and Infrastructure

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  • Media type: E-Article
  • Title: Modules for Experiments in Stellar Astrophysics (MESA): Time-dependent Convection, Energy Conservation, Automatic Differentiation, and Infrastructure
  • Contributor: Jermyn, Adam S.; Bauer, Evan B.; Schwab, Josiah; Farmer, R.; Ball, Warrick H.; Bellinger, Earl P.; Dotter, Aaron; Joyce, Meridith; Marchant, Pablo; Mombarg, Joey S. G.; Wolf, William M.; Sunny Wong, Tin Long; Cinquegrana, Giulia C.; Farrell, Eoin; Smolec, R.; Thoul, Anne; Cantiello, Matteo; Herwig, Falk; Toloza, Odette; Bildsten, Lars; Townsend, Richard H. D.; Timmes, F. X.
  • imprint: American Astronomical Society, 2023
  • Published in: The Astrophysical Journal Supplement Series, 265 (2023) 1, Seite 15
  • Language: Not determined
  • DOI: 10.3847/1538-4365/acae8d
  • ISSN: 0067-0049; 1538-4365
  • Origination:
  • Footnote:
  • Description: <jats:title>Abstract</jats:title> <jats:p>We update the capabilities of the open-knowledge software instrument Modules for Experiments in Stellar Astrophysics (<jats:monospace>MESA</jats:monospace>). The new <jats:monospace>auto</jats:monospace>_<jats:monospace>diff</jats:monospace> module implements automatic differentiation in <jats:monospace>MESA</jats:monospace>, an enabling capability that alleviates the need for hard-coded analytic expressions or finite-difference approximations. We significantly enhance the treatment of the growth and decay of convection in <jats:monospace>MESA</jats:monospace> with a new model for time-dependent convection, which is particularly important during late-stage nuclear burning in massive stars and electron-degenerate ignition events. We strengthen <jats:monospace>MESA</jats:monospace>’s implementation of the equation of state, and we quantify continued improvements to energy accounting and solver accuracy through a discussion of different energy equation features and enhancements. To improve the modeling of stars in <jats:monospace>MESA</jats:monospace>, we describe key updates to the treatment of stellar atmospheres, molecular opacities, Compton opacities, conductive opacities, element diffusion coefficients, and nuclear reaction rates. We introduce treatments of starspots, an important consideration for low-mass stars, and modifications for superadiabatic convection in radiation-dominated regions. We describe new approaches for increasing the efficiency of calculating monochromatic opacities and radiative levitation, and for increasing the efficiency of evolving the late stages of massive stars with a new operator-split nuclear burning mode. We close by discussing major updates to <jats:monospace>MESA</jats:monospace>’s software infrastructure that enhance source code development and community engagement.</jats:p>
  • Access State: Open Access