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Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars
Open accessAbstract
Our understanding of massive star evolution is in flux due to recent upheavals in our view of mass loss and observations of a high binary fraction among O-type stars. Mass-loss rates for standard metallicity-dependent winds of hot stars are lower by a factor of 2–3 compared with rates adopted in modern stellar evolution codes, due to the influence of clumping on observed diagnostics. Weaker hot star winds shift the burden of H-envelope removal to the winds, pulsations, and eruptions of evolved supergiants, as well as binary mass transfer. Studies of stripped-envelope supernovae, in particular, require binary mass transfer. Dramatic examples of eruptive mass loss are seen in Type IIn supernovae, which have massive shells ejected just a few years earlier. These eruptions are a prelude to core collapse, and may signify severe instabilities in the latest nuclear burning phases. We encounter the predicament that the most important modes of mass loss are also the most uncertain, undermining the predictive power of single-star evolution models. Moreover, the influence of winds and rotation has been evaluated by testing single-star models against observed statistics that, it turns out, are heavily influenced by binary evolution. Altogether, this may alter our view about the most basic outcomes of massive-star mass loss—are Wolf-Rayet stars and Type Ibc supernovae the products of winds, or are they mostly the result of binary evolution and eruptive mass loss? This is not fully settled, but mounting evidence points toward the latter. This paradigm shift impacts other areas of astronomy, because it changes predictions for ionizing radiation and wind feedback from stellar populations, it may alter conclusions about star-formation rates and initial mass functions, it affects the origin of compact stellar remnants, and it influences how we use supernovae as probes of stellar evolution across cosmic time.
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“We will also constrain the rates of individual eruption subclasses ( Smith 2014 ) by detecting them in galaxies out to tens of megaparsecs.”
From LSST: From Science Drivers to Reference Design and Anticipated Data Products (2019) · cites this paper as Smith 2014
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Multiwavelength Signatures of Supernova Shock Breakout from Red Supergiants in Two Dimensions
Chen, W.-Y., Chen, K.-J., Maeda, K., Ono, M., Ou, P.-S., & Röpke, F. K. (2026) · The Astrophysical Journal · doi:10.3847/1538-4357/ae3f1e
“The original stellar radii of R20 and R25 are R * = 7.6 × 10 13 cm and R * = 8.3 × 10 13 cm, respectively. on SN shock breakout ( N. Smith 2014 ) .”
InfluentialEnvelope Inflation and Outflow Driven by Energy Deposition in Massive Stars
Mukhija, B., & Kashi, A. (2026) · The Astrophysical Journal · doi:10.3847/1538-4357/ae40c1
“Similar to what has been proposed for pre-SN eruptions (see the review by Smith (2014) and references therein), this explosive outflow phase likely interacts with an extended period of quasi-steady wind-driven outflow.”
Kato, C., Nagakura, H., Ito, A., et al. (2026) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/ae8dc8
“However, theoretical predictions for the final core structure suffer from large uncertainties due to poorly constrained input physics, such as mass-loss rates, binary interactions, and mixing processes (e.g. Smith 2014; Sana et al. 2012; Renzo et al. 2017).”
Wind Accretion in Massive Binaries Experiencing High Mass Loss Rates. II. Eccentricity
Mukhija, B., & Kashi, A. (2026) · Publications of the Astronomical Society of the Pacific · doi:10.1088/1538-3873/ae50bb
“Such conditions are expected in wide O + O and O + WR binaries, luminous blue variable systems, and pre-interaction massive binaries undergoing enhanced wind mass loss ( e.g., Sana et al. 2012; Smith 2014 ) .”
Duan, Y.-L., Tuniyazi, T., & Guo, G. (2026) · Physical review. D/Physical review. D. · doi:10.1103/zvn5-z1yd
Metadata
- Authors
- Smith, N.
- Affiliations
- University of Arizona (US)
- Corresponding author
- Smith, Nathan
- ORCID
- Smith, Nathan
- Venue
- Annual Review of Astronomy and Astrophysics
- Publisher
- Annual Reviews
- Published
- 2014-08-18
- Volume
- 52
- Issue
- 1
- Pages
- 487-528
- ISSN
- 0066-4146 (ISSN-L)
- 1545-4282
- OpenAlex
- W2151213110
- Cited by
- 1,042
- References
- 246
- Citations by year
- 2026: 72 · 2025: 113 · 2024: 94 · 2023: 86 · 2022: 98 · 2021: 82 · 2020: 99 · 2019: 122 · 2018: 76 · 2017: 88 · 2016: 64 · 2015: 40 · 2014: 8
- FWCI
- 4.06
- Type
- journal article
- Language
- en
- Open access
- green
- arxiv.org
- Locations
- Annual Review of Astronomy and Astrophysics (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- arXiv (Cornell University)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Gamma-ray bursts and supernovae
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
- Keywords
- massive star evolution, stellar mass loss, hot star winds, Wolf-Rayet stars, Type Ib/c supernovae, stripped-envelope supernovae, Type IIn supernovae, eruptive mass loss, binary mass transfer, binary star evolution, O-type stars, stellar rotation, stellar feedback
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