The DOI matches its Crossref record; 66 of the 66 references it cites were found in a registry or an index.
Physical Properties of Wolf-Rayet Stars
Open accessAbstract
The striking broad emission line spectroscopic appearance of Wolf-Rayet (WR) stars has long defied analysis, owing to the extreme physical conditions within their line- and continuum-forming regions. Recently, model atmosphere studies have advanced sufficiently to enable the determination of stellar temperatures, luminosities, abundances, ionizing fluxes, and wind properties. The observed distributions of nitrogen- (WN) and carbon (WC)-sequence WR stars in the Milky Way and in nearby star-forming galaxies are discussed; these imply lower limits to progenitor masses of ∼25, 40, and 75 M⊙ for hydrogen-depleted (He-burning) WN, WC, and H-rich (H-burning) WN stars, respectively. WR stars in massive star binaries permit studies of wind-wind interactions and dust formation in WC systems. They also show that WR stars have typical masses of 10–25 M⊙, extending up to 80 M⊙ for H-rich WN stars. Theoretical and observational evidence that WR winds depend on metallicity is presented, with implications for evolutionary models, ionizing fluxes, and the role of WR stars within the context of core-collapse supernovae and long-duration gamma-ray bursts.
Overview
The claims and statistics of this paper haven’t been checked yet.
Run the check — free, no account needed. It reads the open-access text and checks the sources it cites.
Integrity signals
Registry
Cites
Statistics
Verification
Claims the paper makes
The claims and statistics of this paper haven’t been checked yet.
Run the check — free, no account needed. It reads the open-access text and checks the sources it cites.
Self-check
Percentages, sums and reported differences re-computed from the paper’s own numbers.
The self-check needs the paper’s full text.
Citations
Cites
Collapsars: Gamma‐Ray Bursts and Explosions in “Failed Supernovae”
MacFadyen, A. I., & Woosley, S. E. (1999) · The Astrophysical Journal · doi:10.1086/307790 · Cited by 2,328
How Massive Single Stars End Their Life
Heger, A., Fryer, C. L., Woosley, S. E., Langer, N., & Hartmann, D. H. (2003) · The Astrophysical Journal · doi:10.1086/375341 · Cited by 2,165
An unusual supernova in the error box of the γ-ray burst of 25 April 1998
Galama, T. J., Vreeswijk, P. M., van Paradijs, J., Kouveliotou, C., Augusteijn, T., Böhnhardt, H., Brewer, J. P., Doublier, V., Gonzalez, J.-F., Leibundgut, B., et al. (1998) · Nature · doi:10.1038/27150 · Cited by 1,921
The Supernova–Gamma-Ray Burst Connection
Woosley, S. E., & Bloom, J. S. (2006) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev.astro.43.072103.150558 · Cited by 1,766
Interstellar bubbles. II - Structure and evolution
Weaver, R., McCray, R., Castor, J., Shapiro, P., & Moore, R. (1977) · The Astrophysical Journal · doi:10.1086/155692 · Cited by 1,736 · cited 1×
“Ring nebulae provide information on evolutionary links between WR stars and their precursors (Weaver et al. 1977).”
BackgroundRadiation-driven winds in Of stars
Castor, J. I., Abbott, D. C., & Klein, R. I. (1975) · The Astrophysical Journal · doi:10.1086/153315 · Cited by 1,700
A very energetic supernova associated with the γ-ray burst of 29 March 2003
Hjorth, J., Sollerman, J., Møller, P., Fynbo, J. P. U., Woosley, S. E., Kouveliotou, C., Tanvir, N. R., Greiner, J., Andersen, M. I., Castro-Tirado, A. J., et al. (2003) · Nature · doi:10.1038/nature01750 · Cited by 1,498
Shapley, A. E., Steidel, C. C., Pettini, M., & Adelberger, K. L. (2003) · The Astrophysical Journal · doi:10.1086/373922 · Cited by 1,407
Toward Understanding Massive Star Formation
Zinnecker, H., & Yorke, H. W. (2007) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev.astro.44.051905.092549 · Cited by 1,248
The Treatment of Non‐LTE Line Blanketing in Spherically Expanding Outflows
Hillier, D. J., & Miller, D. L. (1998) · The Astrophysical Journal · doi:10.1086/305350 · Cited by 1,151
Cited by
Toward Understanding Massive Star Formation
Zinnecker, H., & Yorke, H. W. (2007) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev.astro.44.051905.092549 · Cited by 1,248
Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars
Smith, N. (2014) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-081913-040025 · Cited by 1,042
“The distance must be known, but the Magellanic Clouds and clusters with known distances can help, and GAIA will soon lower distance uncertainties for the nearest massive stars in the Milky Way.”
BackgroundMethodInfluentialFormation of Double Neutron Star Systems
Tauris, T. M., Kramer, M., Freire, P. C. C., Wex, N., Janka, H.-T., Langer, N., Podsiadlowski, P., Bozzo, E., Chaty, S., Kruckow, M. U., et al. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa7e89 · Cited by 688
Smith, N., Li, W., Filippenko, A. V., & Chornock, R. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.17229.x · Cited by 554
The effect of massive binaries on stellar populations and supernova progenitors
Eldridge, J. J., Izzard, R. G., & Tout, C. A. (2008) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2007.12738.x · Cited by 498
Metadata
- Authors
- Crowther, P. A.
- Venue
- Annual Review of Astronomy and Astrophysics
- Publisher
- Annual Reviews
- Published
- 2007-09-01
- Volume
- 45
- Issue
- 1
- Pages
- 177-219
- ISSN
- 0066-4146 (ISSN-L)
- 1545-4282
- OpenAlex
- W2144755172
- Cited by
- 990
- References
- 66
- FWCI
- 2.94
- Type
- journal article
- Language
- en
- Open access
- green
About these checks
Registry, retraction, Cites and statistics results are computed, not judged, with one exception: a printed reference that no index lists is read once by a model before it counts as a citation error. Claims are extracted by a model and kept only when their quote appears verbatim in the text; each cited source is then checked, with a model’s help, for whether it says what the claim relies on. Those verdicts can be wrong — read the claim’s quote and the cited source before relying on one.
Statistics and arithmetic are recomputed, not judged.
Confidence bands are shown only for fields calibrated on our annotated test set. None is calibrated yet, so no band is shown.
What counts as a claim ›How we measure confidence ›How we check this ›
Are you an author, or do you see a problem with this page? Request a review
How to cite
Cite CoChat for the checks on this page, and the paper for its own findings.
- This page
- CoChat. (2026). Citation check: Physical Properties of Wolf-Rayet Stars. https://app.cochat.ai/papers/10.1146/annurev.astro.45.051806.110615
- The paper
- Crowther, P. A. (2007). Physical Properties of Wolf-Rayet Stars. Annual Review of Astronomy and Astrophysics. https://doi.org/10.1146/annurev.astro.45.051806.110615
Data sources
Bibliographic data: Semantic Scholar, OpenAlex, Crossref.
Contains information from the Semantic Scholar Academic Graph Datasets, made available under the ODC Attribution License (ODC-BY 1.0).
Semantic Scholar’s data is described in: Kinney, R., et al. (2023). The Semantic Scholar Open Data Platform. arXiv:2301.10140.
