{"paper":{"title":"Modules for Experiments in Stellar Astrophysics (MESA): Giant Planets, Oscillations, Rotation, and Massive Stars","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"MESA now models the full evolution of massive stars to core collapse via a new radiation-dominated envelope treatment.","cross_cats":["astro-ph.IM"],"primary_cat":"astro-ph.SR","authors_text":"Aaron Dotter, Bill Paxton, Christopher Mankovich, Dennis Stello, Edward F. Brown, F. X. Timmes, Lars Bildsten, Matteo Cantiello, M. H. Montgomery, Phil Arras, Richard Townsend","submitted_at":"2013-01-02T21:00:00Z","abstract_excerpt":"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 t"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"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 progenitor models.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"The numerical recasting of the Ledoux criterion and the new treatment of radiation-dominated envelopes accurately capture the underlying physics of mixing and envelope structure without introducing significant numerical artifacts or inaccuracies when solving the coupled stellar structure and composition equations.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"MESA Star has been substantially updated with new capabilities for low-mass giant planets, asteroseismology coupling, rotating star models, and uninterrupted massive star evolution to core collapse.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"MESA now models the full evolution of massive stars to core collapse via a new radiation-dominated envelope treatment.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"d2cd054f5a7d57deae589b77529a78cc5cbc1b36c00bfd4bfcf63a1850090b87"},"source":{"id":"1301.0319","kind":"arxiv","version":2},"verdict":{"id":"dc9f1768-deeb-4268-ad8c-cd0ec551661a","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-10T21:36:37.286352Z","strongest_claim":"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 progenitor models.","one_line_summary":"MESA Star has been substantially updated with new capabilities for low-mass giant planets, asteroseismology coupling, rotating star models, and uninterrupted massive star evolution to core collapse.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"The numerical recasting of the Ledoux criterion and the new treatment of radiation-dominated envelopes accurately capture the underlying physics of mixing and envelope structure without introducing significant numerical artifacts or inaccuracies when solving the coupled stellar structure and composition equations.","pith_extraction_headline":"MESA now models the full evolution of massive stars to core collapse via a new radiation-dominated envelope treatment."},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/1301.0319/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"references":{"count":197,"sample":[{"doi":"","year":2011,"title":"2011, A&A, 526, A63","work_id":"3cdd0c49-e641-46c8-a428-9a05381aeb1f","ref_index":1,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2001,"title":"Allard, F., Hauschildt, P. H., Alexander, D. R., Tamanai, A., & Schweitzer, A. 2001, ApJ, 556, 357","work_id":"537ee47d-3250-4de9-b0a2-892ebacc9588","ref_index":2,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2003,"title":"Althaus, L. G., Serenelli, A. M., C´orsico, A. H., & Montgomery, M. H. 2003, A&A, 404, 593","work_id":"7d4457de-d92b-4ca7-a25e-252945b4511e","ref_index":3,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":1999,"title":"1999, Nuclear Physics A, 656, 3","work_id":"7b39823e-86b6-4e7d-9b6d-7756305c6233","ref_index":4,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":1980,"title":"1980, ApJ, 242, 1208","work_id":"a7a5e460-6ed1-4cad-9da7-ddee50e3aef2","ref_index":5,"cited_arxiv_id":"","is_internal_anchor":false}],"resolved_work":197,"snapshot_sha256":"f0273c96cf204b2fe1a194b2734ee753e68740dcd6d47dc46cae1876c1b5a67e","internal_anchors":0},"formal_canon":{"evidence_count":1,"snapshot_sha256":"b83ae542422cd505240426275e1fc1733571fcc663137582aa7c92e16534f386"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}