Dust driven mass loss from carbon stars as a function of stellar parameters - I. A grid of solar-metallicity wind models

@article{Mattsson2010DustDM,
  title={Dust driven mass loss from carbon stars as a function of stellar parameters - I. A grid of solar-metallicity wind models},
  author={Lars Mattsson and Rurik Wahlin and Susanne Hoefner},
  journal={Astronomy and Astrophysics},
  year={2010},
  volume={509},
  pages={13}
}
Context. Knowing how the mass loss of carbon-rich AGB stars depends on stellar parameters is crucial for stellar evolution modelling, as well as for the understanding of when and how circumstellar structures emerge around these stars, e.g., dust shells and so-called detached shells of expelled gas. Aims. The purpose of this paper is to explore the stellar parameter space using a numerical radiation hydrodynamic (RHD) model of carbon-star atmospheres, including a detailed description of dust… 

Dust-driven mass loss from carbon stars as a function of stellar parameters - II. Effects of grain size on wind properties

Context. It is well established that the winds of carbon-rich AGB stars (carbon stars) can be driven by radiation pressure on grains of amorphous carbon and collisional transfer of momentum to the

Synthetic photometry for carbon-rich giants IV. An extensive grid of dynamic atmosphere and wind models ,

Context. The evolution and spectral properties of stars on the asymptotic giant branch (AGB) are significantly affected by mass loss through dusty stellar winds. Dynamic atmosphere and wind models

The origin of carbon: Low-mass stars and an evolving, initially top-heavy IMF?

Carbon is the basis for life, as we know it, but its origin is still largely unclear. Carbon-rich Asymptotic Giant Branch (AGB) stars (carbon stars) play an important role in the cosmic matter cycle

An extensive grid of DARWIN models for M-type AGB stars

Context. The stellar winds of asymptotic giant branch (AGB) stars are commonly attributed to radiation pressure on dust grains, formed in the wake of shock waves that arise in the stellar

Dust Production around Carbon-Rich Stars: The Role of Metallicity

Background: Most of the stars in the Universe will end their evolution by losing their envelope during the thermally pulsing asymptotic giant branch (TP-AGB) phase, enriching the interstellar medium

Carbon star wind models at solar and sub-solar metallicities: a comparative study

Context. The heavy mass loss observed in evolved stars on the asymptotic giant branch (AGB) is usually attributed to dust-driven winds, but it is still an open question how much AGB stars contribute

The mass-loss, expansion velocities, and dust production rates of carbon stars in the Magellanic Clouds

The properties of carbon stars in the Magellanic Clouds (MCs) and their total dust production rates are predicted by fitting their spectral energy distributions (SED) over pre-computed grids of

Estimating the dust production rate of carbon stars in the Small Magellanic Cloud

We employ newly computed grids of spectra reprocessed by dust for estimating the total dust production rate (DPR) of carbon stars in the Small Magellanic Cloud (SMC). For the first time, the grids of

The mass-loss return from evolved stars to the Large Magellanic Cloud - V. The GRAMS carbon-star model grid

The total dust return rate from AGB and RSG star outflows is an important constraint to galactic chemical evolution models. However, this requires detailed radiative transfer (RT) modeling of

Understanding the evolution and dust formation of carbon stars in the Large Magellanic Cloud via the JWST

Context. Carbon stars have been, and still are, extensively studied. Given their complex internal structure and their peculiar chemical composition, they are living laboratories in which we can test
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