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Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation

Paxton, Bill and Smolec, R. and Schwab, Josiah and Gautschy, A. and Bildsten, Lars and Cantiello, Matteo and Dotter, Aaron and Farmer, R. and Goldberg, Jared A. and Jermyn, Adam S. and Kanbur, S. M. and Marchant, Pablo and Thoul, Anne and Townsend, Richard H. D. and Wolf, William M. and Zhang, Michael and Timmes, F. X. (2019) Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation. Astrophysical Journal Supplement Series, 243 (1). Art. No. 10. ISSN 1538-4365. https://resolver.caltech.edu/CaltechAUTHORS:20190709-114116179

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Abstract

We update the capabilities of the open-knowledge software instrument Modules for Experiments in Stellar Astrophysics (MESA). RSP is a new functionality in MESAstar that models the nonlinear radial stellar pulsations that characterize RR Lyrae, Cepheids, and other classes of variable stars. We significantly enhance numerical energy conservation capabilities, including during mass changes. For example, this enables calculations through the He flash that conserve energy to better than 0.001%. To improve the modeling of rotating stars in MESA, we introduce a new approach to modifying the pressure and temperature equations of stellar structure, as well as a formulation of the projection effects of gravity darkening. A new scheme for tracking convective boundaries yields reliable values of the convective core mass and allows the natural emergence of adiabatic semiconvection regions during both core hydrogen- and helium-burning phases. We quantify the parallel performance of MESA on current-generation multicore architectures and demonstrate improvements in the computational efficiency of radiative levitation. We report updates to the equation of state and nuclear reaction physics modules. We briefly discuss the current treatment of fallback in core-collapse supernova models and the thermodynamic evolution of supernova explosions. We close by discussing the new MESA Testhub software infrastructure to enhance source code development.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4365/ab2241DOIArticle
https://arxiv.org/abs/1903.01426arXivDiscussion Paper
ORCID:
AuthorORCID
Smolec, R.0000-0001-7217-4884
Schwab, Josiah0000-0002-4870-8855
Cantiello, Matteo0000-0002-8171-8596
Dotter, Aaron0000-0002-4442-5700
Farmer, R.0000-0003-3441-7624
Goldberg, Jared A.0000-0003-1012-3031
Jermyn, Adam S.0000-0001-5048-9973
Marchant, Pablo0000-0002-0338-8181
Thoul, Anne0000-0002-8107-118X
Townsend, Richard H. D.0000-0002-2522-8605
Wolf, William M.0000-0002-6828-0630
Zhang, Michael0000-0002-0659-1783
Timmes, F. X.0000-0002-0474-159X
Additional Information:© 2019 The American Astronomical Society. Received 2019 March 4; revised 2019 May 15; accepted 2019 May 15; published 2019 July 8. We thank Warrick Ball and Evan Bauer for their sustained engagment with the MESA project. Both Richa Kundu and Susmita Das graciously shared their variable star calculations. It is a pleasure to thank Conny Aerts, Sean Couch, Franck Delahaye, Luc Dessart, Ebraheem Farag, Carl Fields, Chris Fontes, Chris Fryer, Jim Fuller, Sanjib Gupta, Joyce Guzik, Falk Herwig, Thomas Janka, Sam Jones, Max Katz, John Lattanzio, Abhijit Majumder, Wendell Misch, Joey Mombarg, Viktoriya Morozova, Sterl Phinney, Eliot Quataert, Rene Reifarth, Toshio Suzuki, Katie Mussack Tamashiro, Dean Townsley, Todd Thompson, Suzannah Wood, and Mike Zingale for discussions. We also thank the participants of the 2018 MESA Summer School for their willingness to experiment with new capabilities. The improvements discussed in Section 5 were in large part discussed during RHDT and AT stays at the Munger residence. The MESA project is supported by the National Science Foundation (NSF) under the Software Infrastructure for Sustained Innovation program grants (ACI-1663684, ACI-1663688, ACI-1663696). This research benefited from interactions that were funded in part by the Gordon and Betty Moore Foundation through grant GBMF5076 and was also supported at UCSB by the NSF under grant 17-48958. This research was also supported at ASU by the NSF under grant PHY-1430152 for the Physics Frontier Center "Joint Institute for Nuclear Astrophysics—Center for the Evolution of the Elements" (JINA-CEE). Support for this work was provided 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. The Center for Computational Astrophysics at the Flatiron Institute is supported by the Simons Foundation. P.M. acknowledges support from NSF grant AST-1517753 and the Senior Fellow of the Canadian Institute for Advanced Research (CIFAR) program in Gravity and Extreme Universe, both granted to Vassiliki Kalogera at Northwestern University. S.M.K thanks the Indo-US Science and Technology Forum for financial support. A.T. is a Research Associate at the Belgian Scientific Research Fund (F.R.S-FNRS). R.F is supported by the Netherlands Organisation for Scientific Research (NWO) through a top module 2 grant with project No. 614.001.501 (PI de Mink). R.S. acknowledges support from the IdP II 2015 0002 64 grant of the Polish Ministry of Science and Higher Education and from SONATA BIS grant, 2018/30/E/ST9/00598, from the National Science Center, Poland. R.H.D.T. acknowledges support from the NSF under grant AST-1716436. M.Z. was supported by the Heising-Simons Foundation through grant No. 2017-274. J.A.G. is supported by the National Science Foundation Graduate Research Fellowship under grant No. 1650114. A.S.J. acknowledges support from the Gordon and Betty Moore Foundation under grant GBMF7392. This work was in part carried out on the Dutch national e-infrastructure with the support of SURF Cooperative. This paper is based on work supported by the National Aeronautics and Space Administration (NASA) under contract No. NNG16PJ26C issued through the WFIRST Science Investigation Teams Program. This research made extensive use of the SAO/NASA Astrophysics Data System (ADS). Software: gnuplot (Williams & Kelley 2015), ipython/jupyter (Pérez & Granger 2007; Kluyver et al. 2016), matplotlib (Hunter 2007), NumPy (van der Walt et al. 2011), and Python from http://www.python.org.
Funders:
Funding AgencyGrant Number
NSFACI-1663684
NSFACI-1663688
NSFACI-1663696
Gordon and Betty Moore FoundationGBMF5076
NSFPHY-1748958
NSFPHY-1430152
NASA Hubble FellowshipHST-HF2-51382.001-A
NASANAS5-26555
Simons FoundationUNSPECIFIED
NSFAST-1517753
Canadian Institute for Advanced Research (CIFAR)UNSPECIFIED
Indo-US Science and Technology ForumUNSPECIFIED
Fonds de la Recherche Scientifique (FNRS)UNSPECIFIED
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)614.001.501
Ministry of Science and Higher Education (Poland)IdP II 2015 0002 64
Sonata-bis Program2018/30/E/ST9/00598
National Science Centre (Poland)UNSPECIFIED
NSFAST-1716436
Heising-Simons Foundation2017-274
NSF Graduate Research FellowshipDGE-1650114
Gordon and Betty Moore FoundationGBMF7392
NASANNG16PJ26C
Subject Keywords:stars: evolution – stars: general – stars: interiors – stars: oscillations (including pulsations) – stars: rotation – stars: variables: general
Issue or Number:1
Record Number:CaltechAUTHORS:20190709-114116179
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190709-114116179
Official Citation:Bill Paxton et al 2019 ApJS 243 10
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:97001
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:09 Jul 2019 19:53
Last Modified:03 Oct 2019 21:27

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