TY - JOUR
T1 - Modules for Experiments in Stellar Astrophysics (MESA)
T2 - Time-dependent Convection, Energy Conservation, Automatic Differentiation, and Infrastructure
AU - Jermyn, Adam S.
AU - Bauer, Evan B.
AU - Schwab, Josiah
AU - Farmer, R.
AU - Ball, Warrick H.
AU - Bellinger, Earl P.
AU - Dotter, Aaron
AU - Joyce, Meridith
AU - Marchant, Pablo
AU - Mombarg, Joey S.G.
AU - Wolf, William M.
AU - Sunny Wong, Tin Long
AU - Cinquegrana, Giulia C.
AU - Farrell, Eoin
AU - Smolec, R.
AU - Thoul, Anne
AU - Cantiello, Matteo
AU - Herwig, Falk
AU - Toloza, Odette
AU - Bildsten, Lars
AU - Townsend, Richard H.D.
AU - Timmes, F. X.
N1 - Funding Information:
This work used the Extreme Science and Engineering Discovery Environment (XSEDE; Towns et al. ), which is supported by the NSF grant ACI-1548562, specifically Comet at the San Diego Supercomputer Center through allocation TG-AST180050. We thank Charlie Conroy and the Harvard ITC for providing computational resources for continuous testing of MESA through the FASRC Cannon cluster supported by the FAS Division of Science Research Computing Group at Harvard University. J.S. acknowledges use of the lux supercomputer at UC Santa Cruz, funded by NSF MRI grant AST 1828315, and thanks Josh Sonstroem and Brant Robertson for supporting this resource. A.S.J. acknowledges use of the rusty supercomputer at the Flatiron Institute, supported by the Simons Foundation, and thanks the Scientific Computing Core for supporting this resource. W.H.B. thanks the University of Birmingham’s Advanced Research Computing team for support of the BlueBEAR High-Performance Computing service. J.S.G.M. thanks the VSC (Vlaams Supercomputer Centrum—Flemish Supercomputer Center), funded by the Research Foundation—Flanders (FWO) and the Flemish Government—department EWI. T.L.S.W. acknowledges use of computational facilities at UC Santa Barbara funded by NSF grant CNS 1725797, and thanks the Center for Scientific Computing for supporting this resource.
Funding Information:
The MESA Project is supported by the National Science Foundation (NSF) under the Software Infrastructure for Sustained Innovation program grants ACI-1663684, ACI-1663688, and ACI-1663696. This research was supported in part by the NSF under grant No. NSF PHY-1748958 for the Kavli Institute for Theoretical Physics. W.H.B. acknowledges support from the UK Science and Technology Facilities Council (STFC) through grant ST/R0023297/1. G.C.C. acknowledges support by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project No. CE170100013 and the Astronomical Society of Australia. R.F. acknowledges support of the University of Amsterdam’s Helios cluster, which was supported by a European Research Council grant 715063, (PI S.E. de Mink) F.H. acknowledges funding through an NSERC Discovery grant, through NSERC project award SAPPJ-2021-00032 and through the NSF under grant PHY-1430152 for the JINA Center for the Evolution of the Elements. The Flatiron Institute is supported by the Simons Foundation. A.S.J. thanks the Gordon and Betty Moore Foundation (grant GBMF7392) and the National Science Foundation (grant No. NSF PHY-1748958) for supporting this work. M.J. acknowledges the Lasker Data Science Fellowship awarded by the Space Telescope Science Institute, and thanks Marc Pinnsoneault, Jen van Saders, and Jamie Tayar for many hours of consultation on the Yale Rotating Stellar Evolution Code and its documentation. J.S. acknowledges support by NASA through Hubble Fellowship grant No. HST-HF2-51382.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555, by the A. F. Morrison Fellowship in Lick Observatory, and by the National Science Foundation through grant ACI-1663688. R.S. acknowledges support by the National Science Center, Poland, Sonata BIS project 2018/30/E/ST9/00598. A.T. is a Research Associate at the Belgian Scientific Research Fund (F.R.S.-F.N.R.S.). F.X.T. acknowledges support by NASA under the Astrophysics Theory Program grant NNH21ZDA001N-ATP, and by the NSF under grant PHY-1430152 for the JINA Center for the Evolution of the Elements. T.L.S.W. thanks support by the Gordon and Betty Moore Foundation through grant GBMF5076. J.S.G.M. acknowledges support by the KU Leuven Research Counsil (grant C16/18/005: PARADISE). O.T. was supported by a FONDECYT project 321038. P.M. acknowledges support from the FWO junior postdoctoral fellowship No. 12ZY520N. This research made extensive use of the SAO/NASA Astrophysics Data System (ADS).
Publisher Copyright:
© 2023. The Author(s). Published by the American Astronomical Society.
PY - 2023/3/1
Y1 - 2023/3/1
N2 - We update the capabilities of the open-knowledge software instrument Modules for Experiments in Stellar Astrophysics (MESA). The new auto_diff module implements automatic differentiation in MESA, 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 MESA 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 MESA’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 MESA, 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 MESA’s software infrastructure that enhance source code development and community engagement.
AB - We update the capabilities of the open-knowledge software instrument Modules for Experiments in Stellar Astrophysics (MESA). The new auto_diff module implements automatic differentiation in MESA, 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 MESA 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 MESA’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 MESA, 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 MESA’s software infrastructure that enhance source code development and community engagement.
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U2 - 10.3847/1538-4365/acae8d
DO - 10.3847/1538-4365/acae8d
M3 - Article
AN - SCOPUS:85149144782
SN - 0067-0049
VL - 265
JO - Astrophysical Journal, Supplement Series
JF - Astrophysical Journal, Supplement Series
IS - 1
M1 - 15
ER -