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Systematic survey of the effects of wind mass loss algorithms on the evolution of single massive stars

Renzo, M. and Ott, C. D. and Shore, S. N. and de Mink, S. E. (2017) Systematic survey of the effects of wind mass loss algorithms on the evolution of single massive stars. Astronomy and Astrophysics, 603 . Art. No. A118. ISSN 0004-6361. http://resolver.caltech.edu/CaltechAUTHORS:20170901-125621395

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Abstract

Mass loss processes are a key uncertainty in the evolution of massive stars. They determine the amount of mass and angular momentum retained by the star, thus influencing its evolution and presupernova structure. Because of the high complexity of the physical processes driving mass loss, stellar evolution calculations must employ parametric algorithms, and usually only include wind mass loss. We carried out an extensive parameter study of wind mass loss and its effects on massive star evolution using the open-source stellar evolution code MESA. We provide a systematic comparison of wind mass loss algorithms for solar-metallicity, nonrotating, single stars in the initial mass range of 15 M⊙ to 35 M⊙. We consider combinations drawn from two hot phase (i.e., roughly the main sequence) algorithms, three cool phase (i.e., post-main-sequence) algorithms, and two Wolf-Rayet mass loss algorithms. We discuss separately the effects of mass loss in each of these phases. In addition, we consider linear wind efficiency scale factors of 1, 0.33, and 0.1 to account for suggested reductions in mass loss rates due to wind inhomogeneities. We find that the initial to final mass mapping for each zero-age main-sequence (ZAMS) mass has a ~ 50% uncertainty if all algorithm combinations and wind efficiencies are considered. The ad-hoc efficiency scale factor dominates this uncertainty. While the final total mass and internal structure of our models vary tremendously with mass loss treatment, final luminosity and effective temperature are much less sensitive for stars with ZAMS mass ≲ 30 M⊙. This indicates that uncertainty in wind mass loss does not negatively affect estimates of the ZAMS mass of most single-star supernova progenitors from pre-explosion observations. Our results furthermore show that the internal structure of presupernova stars is sensitive to variations in both main sequence and post main-sequence mass loss. The compactness parameter ξ ∝ ℳ /R(ℳ) has been identified as a proxy for the “explodability” of a given presupernova model. We find that ξ varies by as much as 30% for models of the same ZAMS mass evolved with different wind efficiencies and mass loss algorithm combinations. This suggests that the details of the mass loss treatment might bias the outcome of detailed core-collapse supernova calculations and the predictions for neutron star and black hole formation.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1051/0004-6361/201730698DOIArticle
https://www.aanda.org/articles/aa/abs/2017/07/aa30698-17/aa30698-17.htmlPublisherArticle
https://arxiv.org/abs/1703.09705arXivDiscussion Paper
ORCID:
AuthorORCID
Ott, C. D.0000-0003-4993-2055
Additional Information:© 2017 ESO. Article published by EDP Sciences. Received 24 February 2017; Accepted 28 March 2017; Published online 18 July 2017. We wish to thank B. Paxton, F. Timmes, and R. Farmer for invaluable help with MESA. We acknowledge helpful exchanges with W. D. Arnett, M. Cantiello, D. Clausen, A. de Koter, L. Dessart, Y. Götberg, A. L. Piro, J. Fuller, N. Smith, and E. Zapartas. We are also grateful to the referee, G. Meynet, for the helpful comments and suggested improvements. M.R. thanks the University of Pisa, where this study was initiated as part of his Master Thesis in Physics, and acknowledges the precious support of the “Lorentz group”. This work is supported in part by NSF under grant numbers AST-1205732, AST-1212170, PHY-1151197, and PHY-1125915 and by the Sherman Fairchild Foundation. Some of the computations used resources of NSF’s XSEDE network under allocation TG-PHY100033. Most of the simulation were carried out using the Caltech compute cluster Zwicky funded through NSF grant no. PHY-0960291 and the Sherman Fairchild Foundation. The runs to the onset of core collapse were carried out on the Dutch national e-infrastructure (Cartesius, project number 15162) with the support of the SURF Cooperative.
Group:TAPIR, Walter Burke Institute for Theoretical Physics
Funders:
Funding AgencyGrant Number
NSFAST-1205732
NSFAST-1212170
NSFPHY-1151197
NSFPHY-1125915
Sherman Fairchild FoundationUNSPECIFIED
NSFTG-PHY100033
NSFPHY-0960291
Subject Keywords:stars: evolution – stars: massive – stars: mass-loss – stars: winds, outflows – supernovae: general
Record Number:CaltechAUTHORS:20170901-125621395
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20170901-125621395
Official Citation:Systematic survey of the effects of wind mass loss algorithms on the evolution of single massive stars M. Renzo, C. D. Ott, S. N. Shore and S. E. de Mink A&A, 603 (2017) A118 DOI: https://doi.org/10.1051/0004-6361/201730698
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:81077
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:01 Sep 2017 20:09
Last Modified:01 Sep 2017 20:09

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