Radiation driven winds of hot luminous stars - XIV. Line statistics and radiative driving

By J. Puls, U. Springmann, M. Lennon. 2000

134 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Mechanics of Materials

View Paper: https://www.semanticscholar.org/paper/4731945c5522f6ce02d6cb8afecf6cd7736a7a88

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Citations in the corpus

Line-driven Winds, Ionizing Fluxes, and Ultraviolet Spectra of Hot Stars at Extremely Low Metallicity. I. Very Massive O Stars (2002, methodology): “The calculations, which are very similar to those carried out by Kudritzki et al. (1998) and Puls et al. (2000), use a program code developed by U. Springmann during his thesis work (see Springmann 1997).”
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, background): “…weak dependence upon the effective temperature and metallicity (and in a way that can be theoretically predicted from radiativedriven wind theory; see Puls et al. 2000, Kudritzki 2002, as well as Vink et al. 2000, 2001, but see also Martins et al. 2004 for counter-examples) one can in fact use Eq.”
Mass loss from hot massive stars (2008, background): “2 M−1.3 Teff (v∞/vesc)−1.3.”
Massive Stars in the Local Group: Implications for Stellar Evolution and Star Formation (2003, background): “However, this deceptively simple expression hides much of the complication, sinceα depends upon the effective temperature andZ in a manner that can only be determined by detailed modeling (Kudritzki & Puls 2000, Puls et al. 2000).”
On the Spectral Evolution of Hot White Dwarf Stars. I. A Detailed Model Atmosphere Analysis of Hot White Dwarfs from SDSS DR12 (2020, background): “As the strength of metaldriven winds depends mostly on the luminosity (Puls et al. 2000), the cooling causes the wind to cease and thus the contaminants to settle: ultimately, homogeneous DAO stars become genuine DA stars.”
O stars with weak winds: the Galactic case (2005, background): “A nice possibility was highlighted by Puls et al. (2000) in their very detailed analysis of the line statistics.”
Mass loss from late-type WN stars and its Z-dependence: very massive stars approaching the Eddington limit (2008, background): “Note thatα also reflects the relative contribution of optically thick spectral lines to the overall wind driving (see, e.g. Puls et al. 2000).”
Stellar and wind parameters of Galactic O-stars - The influence of line-blocking/blanketing (2004, background): “In summary, the calculation of the required NLTE metal opacities (bound-bound, bound-free, and freefree) follows the principal philosophy presented by Abbott & Lucy (1985), Schmutz (1991), Schaerer & Schmutz (1994) and Puls et al. (2000) and important details have now been improved upon.”
The empirical metallicity dependence of the mass-loss rate of O- and early B-type stars (2007, background): “The reason is that log D◦ contains a term ∝(3/2− x) log M, which (almost) vanishes since x happens to be ∼3/2 for O-stars and early B-supergiants (Puls et al. 2000).”