Mass Loss from Cool Stars: Impact on the Evolution of Stars and Stellar Populations

By L. Willson. 2000

213 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/66c6e967cf751f66ccb95336e5676554aaa76b18

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In Astronomy and Astrophysics

Citations in the corpus

The second and third parameters of the horizontal branch in globular clusters (2010, background): “Unfortunately, the physics of mass loss is very poorly known at present (see e.g., Willson 2000; Meszeros et al. 2009; Dupree et al. 2009).”
THE ACS NEARBY GALAXY SURVEY TREASURY. IX. CONSTRAINING ASYMPTOTIC GIANT BRANCH EVOLUTION WITH OLD METAL-POOR GALAXIES (2010, methodology): “…the star enters the dustdriven wind regime, which is treated according to two formalisms: • case A: based on Bowen & Willson (1991), but relaxing the metallicity dependence suggested by Willson (2000); • case B: based on Bedijn (1988), but with a somewhat different calibration of the parameters.”
A New Version of Reimers’ Law of Mass Loss Based on a Physical Approach (2005, unknown): “For further updated information on mass-loss mechanisms see, e.g., the review by Willson (2000).”
Super and massive AGB stars - IV. Final fates - Initial to final mass relation (2014, background): “Whilst traditionally the mass-loss rate was thought to be lower at low metallicity (e.g. Bowen & Willson 1991; Willson 2000; Zijlstra 2004), recent theoretical (e.g. Mattsson et al. 2008) and observational (e.g. Groenewegen et al. 2009; Lagadec & Zijlstra 2008) studies suggest this may not always…”
Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars (2014, background): “RSG mass loss is time dependent, and there appears to be a wide dispersion even for a given luminosity and temperature (Willson 2000).”
Constraining the thermally pulsing asymptotic giant branch phase with resolved stellar populations in the Large Magellanic Cloud (2019, background): “The abundant literature on the topic proves that over the years substantial efforts have been devoted to understand the physical mechanisms responsible for mass-loss in AGB stars, and more generally in red giants (see Höfner & Olofsson 2018; Willson 2000 for extensive reviews).”
TESTING A PREDICTIVE THEORETICAL MODEL FOR THE MASS LOSS RATES OF COOL STARS (2011, background): “The outer atmospheres of cool stars are also likely to be powered by acoustic or longitudinal MHD waves (Cuntz 1990; Buchholz et al. 1998), episodic flares or coronal mass ejections (Mullan 1996; Aarnio et al. 2009), and large-amplitude pulsations (Bowen 1988; de Jager et al. 1997; Willson 2000).”
FORETELLINGS OF RAGNARÖK: WORLD-ENGULFING ASYMPTOTIC GIANTS AND THE INHERITANCE OF WHITE DWARFS (2012, background): “The Reimers relation for the AGB phase does not agree with observations through the entire AGB phase: it gives mass-loss rates that increase too slowly, take too long, and reach values too small (see e.g. Willson 2000; Bowen & Willson 1991).”
Stellar evolution with rotation. VII. - Low metallicity models and the blue to red supergiant ratio in the SMC (2001, background): “For the red supergiants, there are a number of recent parametrizations proposed (cf. Willson 2000), from low to high rates.”
Modeling the Panchromatic Spectral Energy Distributions of Galaxies (2013, background): “8M⊙) it is believed to be due to pulsation-induced dust-driven winds (Willson 2000).”
Dust formation in early galaxies (2003, background): “We have followed the evolutionary model grids in † Dust driven winds only become important at high metallicities where there is sufficient dust production to drive the gas outwards (Willson 2000).”
Evolution of asymptotic giant branch stars. I. Updated synthetic TP-AGB models and their basic calibration (2007, background): “The theoretical modelling of the mass-loss phenomenon has also significantly improved (Willson 2000; Winters et al. 2003; Article published by EDP Sciences and available at http://www.aanda.org or http://dx.doi.org/10.1051/0004-6361:20066772 Höfner et al. 2003, and references therein).”
Evolution of Asymptotic Giant Branch Stars (2005, background): “Several aspects or related issues have been covered since by review articles in this series, like mass loss (Willson 2000), the s process (Busso, Gallino & Wasserburg 1999; Meyer 1994), and the A nn u.”
Mass loss of stars on the asymptotic giant branch (2018, background): “Willson (2000) gives a detailed analysis of problems in deriving a “mass-loss formula”, i.e., a quantitative description of how the mass-loss rate depends on fundamental stellar parameters, as used in evolution models.”
MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, background): “However, we emphasize that these are still empirically motivated recipes and therefore remain agnostic on the subject of the actual mechanism driving the winds (see a review by Willson 2000 for a discussion on, e.g., dust-driven winds).”