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- W28921875 abstract "Intermediate mass stars contribute to the enrichment of the interstellar medium via mass-loss of the order of up to several 10−5 Msun yr−1 during their evolution along the Asymptotic Giant Branch. As driving mechanism radiation pressure on dust grains formed in the cool atmospheres of these stars plays an important role. The stellar pulsation results in a levitation of the atmosphere, pushing the atmospheric gas into the dust formation window, a thermodynamic regime where density and temperature are favourable for grain formation. Radiation pressure then accelerates the dust particles and the surrounding gas is dragged along via frictional coupling, generating those massive outflows. In our work, we are interested in the total mass lost by stellar samples with subsolar metallicities. In order to give a quantitative account, a description of the mass loss is needed which can be applied to stellar evolution calculations. Following the approach for solar metallicity stars we derive the mass-loss description from hydrodynamical wind models for long-period variables. The models have been adapted to the lower opacity, which is to be expected because of the low metallicity. This modification involves a proper description of the transport of radiation through a medium of arbitrary optical thickness. In this contribution we present results obtained from models calculated with abundances as found in the Large Magellanic Cloud. The mass-loss history of single stars is examined as well as their integrated mass loss." @default.
- W28921875 created "2016-06-24" @default.
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- W28921875 date "2006-01-01" @default.
- W28921875 modified "2023-10-03" @default.
- W28921875 title "Mass loss of dust-driven winds at subsolar metallicity ." @default.
- W28921875 hasPublicationYear "2006" @default.
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