A Tale of Two Stars: The Extreme O7 Iaf+ Supergiant AV 83 and the OC7.5 III((f)) star AV 69

By D. John Hillier, T. Lanz, S. Heap, I. Hubeny, Linda J. Smith, Christopher H. Evans, D. Lennon, J. Bouret. 2003

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In Astronomy and Astrophysics

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Atmospheric NLTE-models for the spectroscopic analysis of blue stars with winds. II. Line-blanketed models (2004, background): “These include (i) spatially constant clumping factors from a predefined velocity on, (ii) the default parameterization of cmfgen (Hillier & Miller 1999, Hillier et al. 2003), and (iii) generalizations of the latter (see Najarro et al. 2011).”
The empirical metallicity dependence of the mass-loss rate of O- and early B-type stars (2007, methodology): “…O stars are also clumped was provided by Eversberg et al. (1998) from time series spectroscopy of He ii λ4686 in ζ Pup, and by Crowther et al. (2002); Hillier et al. (2003); Bouret et al. (2003); Massa et al. (2003); Martins et al. (2004, 2005); Bouret et al. (2005), and Fullerton et al. (2006)…”
Mass loss from hot massive stars (2008, methodology): “Howarth and Prinja (1989) and Prinja et al (1990) have used this asymp totic value”
On the Role of Continuum-driven Eruptions in the Evolution of Very Massive Stars and Population III Stars (2006, background): “…traditional mass-loss rates, while Bouret et al. (2005) require reductions by factors of 3 or more (see also Puls et al. 2006; Crowther et al. 2002; Hillier et al. 2003; Massa et al. 2003; Evans et al. 2004).3 In any case, large reductions in Ṁ are also needed to match the unexpectedly symmetric…”
Bright OB stars in the Galaxy. III. Constraints on the radial stratification of the clumping factor (2006, result): “Accounting for these findings and other investigations with similar results (e.g., Hillier et al. 2003; Bouret et al. 2003), there seems to be increasing evidence that the agreement between the theoretical and observed WLR (which, if real, would imply a smooth wind in the radio regime) is indeed…”
The most massive stars in the Arches cluster (2007, background): “As previously recalled, we note however that recent studies indicate smallerf for O supergiants (Crowther et al. 2002a; Hillier et al. 2003; Bouret et al. 2005).”
Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars (2014, methodology): “For the Milky Way, LMC, and SMC, various studies using modern non-LTE analysis find fcl ≃ 10 (Crowther et al. 2002, Evans et al. 2004, Figer et al. 2002, Hillier et al. 2003, Massa et al. 2003, Puls et al. 2006), corresponding to Ṁ reductions by a factor of ∼3 with typical uncertainties of ∼30%.”
The Discordance of Mass-Loss Estimates for Galactic O-Type Stars (2005, background): “The values of f1 derived from detailed spectroscopic fits to O stars in the Small Magellanic Cloud are typically 0.1 (Crowther et al. 2002; Hillier et al. 2003; Bouret et al. 2003; Evans et al. 2004).”
Stellar and wind parameters of Galactic O-stars - The influence of line-blocking/blanketing (2004, background): “…recent UV-analyses and the problematic line cores of the blue Balmer lines, see above, with additional support from a recent investigation by Hillier et al. (2003)) we have argued that the different WLRs can be unified on the basis of the following assumptions: For those stars with Hα in…”
UBVJHK synthetic photometry of Galactic O stars (2006, background): “…allows realistic prediction of atmospheric structures andemergent spectra which are used to get quantitative constraints on the properties of massive stars (Crowther et al., 2002; Hillier et al., 2003; Bouret et al., 2003; Martins et al., 2004; Repolust, Puls & Herrero, 2004; Martins et al., 2005).”
The Physical Properties and Effective Temperature Scale of O-Type Stars as a Function of Metallicity. II. Analysis of 20 More Magellanic Cloud Stars and Results from the Complete Sample (2005, methodology): “This was partially corrected by a re-reduction of the data for the versions used by Hillier et al. (2003), Bouret et al. (2003), and Heap et al. (2005), although no correction could be made for NGC 346-368 or NGC346-487 since there weren’t enough sky pixels.”
Lower mass loss rates in O-type stars: Spectral signatures of dense clumps in the wind of two Galactic O4 stars (2004, methodology): “Hillier et al. (2003) achieved a good match to the observed P doublet in the SMC O7Iaf+ supergiant AV 83 with homogeneous wind models using a low abundance P/P⊙ = 0.04 (compared to the adopted overall SMC metallicity, Z/Z⊙ = 0.2).”
The R136 star cluster dissected with Hubble Space Telescope/STIS. I. Far-ultraviolet spectroscopic census and the origin of He II λ1640 in young star clusters (2016, background): “It is well known that mass-loss rates of O stars at a given temperature and luminosity span a wide range of values (Hillier et al. 2003).”
The VLT-FLAMES Survey of Massive Stars: Observations in the Galactic Clusters NGC 3293, NGC 4755 and NGC 6611 ⋆ (2005, methodology): “Results from model atmosphere analyses of O- and B-type supergiants in the Magellanic Clouds (Crowther et al. 2002; Bouret et al. 2003; Hillier et al. 2003; Evans et al. 2004a; Trundle et al. 2004; Walborn et al. 2004; Trundle & Lennon 2005) find evidence of significant nitrogen enrichment, that…”
Stellar and wind properties of massive stars in the central parsec of the Galaxy (2006, background): “To name a few, their effective temperatures are lower (Martins et al. 2002; Crowther et al. 2002; Repolust et al. 2004) and their winds are highly clumped (Hillier et al. 2003; Bouret et al. 2005; Fullerton et al. 2006).”
Physical parameters and wind properties of galactic early B supergiants (2005, methodology): “In the present application, we have utilized CMFGEN, the current version of which is discussed by Hillier et al. (2003).”
Quantitative Spectroscopy of O Stars at Low Metallicity: O Dwarfs in NGC 346 (2003, methodology): “Hillier et al. (2003) have presented a detailed discussion of this issue for AV 83.”
A new calibration of stellar parameters of Galactic O stars (2005, background): “However, other recent analysis show that consistent results with good fits can be obtained for photospheric UV and optical lines (Bouret et al. 2003, Hillier et al. 2003, Martins et al. 2005).”
Mass loss from late-type WN stars and its Z-dependence: very massive stars approaching the Eddington limit (2008, background): “The reason for this is not yet fully understood (but see the discus ion in Hillier et al. 2003).”
O stars with weak winds: the Galactic case (2005, methodology): “…several studies of supergiants in the Magellanic Clouds using FUSE + optical data do not reveal any problem with the CMFGEN wind ionisation fractions, except that clumping must be used to reproduce a couple of (but not all) lines (see Crowther et al. 2002, Hillier et al. 2003, Evans et al. 2004).”