From wind to superwind - The evolution of mass-loss rates for Mira models

Bowen, G. H.; Willson, L. A.

doi:10.1086/186086

Cited by 178 publications

(204 citation statements)

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“…However, over the years, it has become clear that the Reimers law is not suitable to describe the efficiency of mass loss on the AGB, as this formula does not account for the observed steep increase of the mass-loss rate at increasing luminosity, as shown by studies of mass-losing pulsating AGB stars Vassiliadis & Wood (1993). Many other formalisms/recipes for AGB mass loss have been proposed, either semi-empirical (van Loon et al 2005;Groenewegen et al 1998;Vassiliadis & Wood 1993), or derived from hydrodynamic dust-driven pulsationassisted wind models (Mattsson et al 2010;Wachter et al 2008Wachter et al , 2002Arndt et al 1997;Bloecker 1995;Bowen & Willson 1991;Bedijn 1988).…”

Section: Predicted Ifmr: Basic Dependenciesmentioning

confidence: 99%

Asymptotic Giant Branch Evolution and the Initial-Final Mass Relation of Single CO White Dwarfs

Marigo¹

2011

Proc. IAU

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Abstract. Combining recent mass determinations of Galactic CO white dwarfs and their progenitors with the latest evolutionary models for Asymptotic Giant Branch (AGB) stars, I review the initial-final mass relation (IFMR) of low-and intermediate-mass stars. In particular, I analyze the impact on the IFMR produced by a few critical processes characterizing the AGB phase, namely: the second and third dredge-up events, hot-bottom burning, and mass loss. Their dependence on metallicity and related theoretical uncertainties are briefly discussed.

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Section: Predicted Ifmr: Basic Dependenciesmentioning

confidence: 99%

Asymptotic Giant Branch Evolution and the Initial-Final Mass Relation of Single CO White Dwarfs

Marigo¹

2011

Proc. IAU

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“…Many studies also assume some continuous mass loss, speci ed by the Reimers relation (with a suitable tting parameter), followed at the end of the AGB by a \superwind" with a steeper dependence of mass loss on stellar parameters. Detailed models of pulsating stars (Bowen & Willson 1991;Willson et al 1996) demonstrate the inadequacy of simple parametrizations | the mass loss rate turns out to bequite sensitive to stellar parameters, including mass and composition, and this cannot be determined empirically from available observed mass loss rates because the stellar parameters are not well known.…”

Section: Introductionmentioning

confidence: 99%

Carbon Stars and Nucleosynthesis in Galaxies

Gustafsson¹,

Ryde²

2000

Symp. - Int. Astron. Union

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Abstract. The role of carbon stars in the build-up of chemical elements in galaxies is discussed on the basis of stellar evolution calculations and estimated stellar yields, abundance analyses of AGB stars, galactic-evolution models and abundance trends among solar-type disk stars. We conclude that the AGB stars in general, and carbon stars in particular, probably are main contributors of s-elements, that their contributions of ourine and carbon are quite signi cant, and that possibly their contributions of lithium, 13 C and 22 Ne are of some importance. Also contributions of N, Na and Al are discussed. The major uncertainties that characterize almost any statement concerning these issues are underlined.

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“…It has been proposed (e.g. Bedijn 1988;Willson 1991) that the mass-loss rate actually increases with time so that a star loses a good share of its mass near the end of the AGB evolution, its envelope being finally stripped away.…”

Section: Introductionmentioning

confidence: 99%

“…Models for pulsating red giant stars have been able to incorporate a great deal of physics in describing the atmospheric structure and stellar winds from Luminous Red Variables, or LRVs (Bowen & Willson 1991). However, these impressive models assume spherical symmetry, despite the fact that departures from spherical symmetry are known to exist around LRVs.…”

Section: Introductionmentioning

confidence: 99%

Asymmetries around Luminous Red Variables

Magalhães

Nordsieck

2000

Symp. - Int. Astron. Union

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Abstract. Departures from spherical symmetry are known to exist around Luminous Red Variables (LRVs). One of the earliest pieces of evidence came from the discovery that light from these objects is polarized. Additional evidence comes from other techniques and observations of related objects. This talk briefly reviews these data and focuses on the mechanisms that produce polarization in LRVs. Emphasis is given on recent spectropolarimetric monitoring data of selected key objects and what we have learned about the LRV environment from such data.

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From wind to superwind - The evolution of mass-loss rates for Mira models

Cited by 178 publications

References 0 publications

Asymptotic Giant Branch Evolution and the Initial-Final Mass Relation of Single CO White Dwarfs

Asymptotic Giant Branch Evolution and the Initial-Final Mass Relation of Single CO White Dwarfs

Carbon Stars and Nucleosynthesis in Galaxies

Asymmetries around Luminous Red Variables

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