WINDS FROM HOT STARS

By R. Kudritzki, J. Puls. 2000

565 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/ceb252a2f318b26127c7c611659b209632c0f932

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In Astronomy and Astrophysics

1. Michela Mapelli
2. N. Smith
3. P. Hopkins
4. S. Smartt
5. L. Hernquist
6. N. Giacobbo
7. C. Conroy
8. N. Langer

Citations in the corpus

• Fast rotating massive stars and the origin of the abundance patterns in galactic globular clusters (2006, background): “The radiative mass loss rates are from Kudritzki & Puls (2000) when log Teff > 3.95 and from de Jager et al. (1988) otherwise.”
• Quantitative Spectroscopy of O Stars at Low Metallicity: O Dwarfs in NGC 346 (2003, background): “Winds from massive stars are radiatively driven through the transfer of momentum from the stellar radiation field to the atmospheric material via photon absorptions and scattering due to thousands of metal lines (Castor, Abbott, & Klein 1975; Kudritzki & Puls 2000).”
• Theoretical Challenges in Galaxy Formation (2016, background): “Radiation driven stellar winds from O- and B-stars (Castor, Abbott & Klein 1975; Kudritzki & Puls 2000; Puls et al. 1996) create bubbles of low density gas around the stars.”
• Carnegie Supernova Project: Observations of Type IIn supernovae ⋆ (2013, background): “CSI occurs when the SN blast-wave shocks circumstellar material (CSM) (e.g. Chugai & Danziger 1994; Fransson et al. 2002), which originates in prevalent winds and/or violent eruptions of the progenitors during their pre-SN evolutionary phase (Kudritzki & Puls 2000).”
• Observed Fractions of Core-Collapse Supernova Types and Initial Masses of their Single and Binary Progenitor Stars (2010, background): “Massive stars have substantial steady stellar winds through most of their lives (see Lamers & Cassinelli 1999), with either metallicity-dependent, line-driven winds in hot stars (Kudritzki & Puls 2000), or slow, pulsation/dust-driven winds in cool stars (Reimers 1977).”
• PARSEC evolutionary tracks of massive stars up to 350 M ☉ at metallicities 0.0001 ≤ Z ≤ 0.04 (2015, background): “…amount of their mass through line-driven stellar winds and that the mass-loss rates show a simple scaling law with the metallicity (Castor, Abbott & Klein 1975; Kudritzki & Puls 2000; Nugis & Lamers 2000; Vink, de Koter & Lamers 2000, 2001; Muijres et al. 2012b; Crowther 2007; Smith 2014).”
• Progenitor mass constraints for core-collapse supernovae from correlations with host galaxy star formation⋆ (2012, background): “…are expected on theoretical grounds as at higher metallicity progenitor stars have higher mass-loss rates through radiatively driven winds (see e.g. Puls et al. 1996; Kudritzki & Puls 2000; Mokiem et al. 2007) and hence it is easier for a star to lose its outer envelopes and explode as an SNIbc.”
• RECONCILING THE STELLAR AND NEBULAR SPECTRA OF HIGH-REDSHIFT GALAXIES (2016, background): “…end states, and chemical yields from massive stars all depend on the details of mass loss (e.g., Smith 2014), which itself depends on the initial chemical composition (e.g., Puls et al. 2008; Kudritzki & Puls 2000; Cantiello et al. 2007; Eldridge et al. 2011; Brott et al. 2011; Langer 2012).”
• Massive Stars in the Local Group: Implications for Stellar Evolution and Star Formation (2003, background): “For O-type stars, the value ofα is approximately 0.6 (Pauldrach et al. 1986, Kudritzki & Puls 2000), suggesting a luminosity exponent ∼1.7, similar to what is observed.”
• Formation of Supermassive Black Hole Seeds (2016, background): “…show that mass loss from the stellar winds is metallicity dependent, scales with ṁloss ∝ Z 0.5 and consequently metal rich stars show much higher mass loss compared to the metal poor stars (Nugis & Lamers 2000; Kudritzki & Puls 2000; Baraffe et al. 2001; Heger et al. 2003; Meynet & Maeder 2005).”
• Formation of Double Neutron Star Systems (2017, background): “The observational and theoretical estimated values depend on the modelling of the terminal wind velocity, clumping effects, metallicity and absorption properties in the local environment (Kudritzki & Puls 2000; Vink et al. 2001; Repolust et al. 2004; Crowther et al. Notes —”
• Physical Properties of Wolf-Rayet Stars (2006, background): “Although numbers are small, this downward trend in wind velocity with decreasing metallicity is believed to occur for other O and WR spectral types (e.g. Kudritzki & Puls 2000; Crowther 2000).”
• Physical parameters and wind properties of galactic early B supergiants (2005, result): “Galactic B supergiants from Lamers et al. (1995) together with the Kudritzki & Puls (2000) scalings (dotted lines);(lower panel): Galactic B supergiants from the present study (filled circles), together with results from Evans et al. (2004a, open triangles) for SMC B supergiants.”
• Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars (2014, background): “A previous review by Kudritzki & Puls (2000) (KP00 hereafter) dealt with line-driven winds of hot stars, focussing on the theory of the driving mechanism as well as common scaling relations used to convert observables to rates.”