Three-component modelling of C-rich AGB star winds V. Effects of frequency-dependent radiative transfer including drift. (arXiv:2006.11296v2 [astro-ph.SR] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Sandin_C/0/1/0/all/0/1">Christer Sandin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mattsson_L/0/1/0/all/0/1">Lars Mattsson</a>
Stellar winds of cool carbon stars enrich the interstellar medium with
significant amounts of carbon and dust. We present a study of the influence of
two-fluid flow on winds where we add descriptions of frequency-dependent
radiative transfer. Our radiation hydrodynamic models in addition include
stellar pulsations, grain growth and ablation, gas-to-dust drift using one mean
grain size, dust extinction based on both the small particle limit and Mie
scattering, and an accurate numerical scheme. We calculate models at high
spatial resolution using 1024 gridpoints and solar metallicities at 319
frequencies, and we discern effects of drift by comparing drift models to
non-drift models. Our results show differences of up to 1000 per cent in
comparison to extant results. Mass-loss rates and wind velocities of drift
models are typically, but not always, lower than in non-drift models.
Differences are larger when Mie scattering is used instead of the small
particle limit. Amongst other properties, the mass-loss rates of the gas and
dust, dust-to-gas density ratio, and wind velocity show an exponential
dependence on the dust-to-gas speed ratio. Yields of dust in the least massive
winds increase by a factor four when drift is used. We find drift velocities in
the range 10-67 km/s, which is drastically higher than in our earlier works
that use grey radiative transfer. It is necessary to include an estimate of
drift velocities to reproduce high yields of dust and low wind velocities.
Stellar winds of cool carbon stars enrich the interstellar medium with
significant amounts of carbon and dust. We present a study of the influence of
two-fluid flow on winds where we add descriptions of frequency-dependent
radiative transfer. Our radiation hydrodynamic models in addition include
stellar pulsations, grain growth and ablation, gas-to-dust drift using one mean
grain size, dust extinction based on both the small particle limit and Mie
scattering, and an accurate numerical scheme. We calculate models at high
spatial resolution using 1024 gridpoints and solar metallicities at 319
frequencies, and we discern effects of drift by comparing drift models to
non-drift models. Our results show differences of up to 1000 per cent in
comparison to extant results. Mass-loss rates and wind velocities of drift
models are typically, but not always, lower than in non-drift models.
Differences are larger when Mie scattering is used instead of the small
particle limit. Amongst other properties, the mass-loss rates of the gas and
dust, dust-to-gas density ratio, and wind velocity show an exponential
dependence on the dust-to-gas speed ratio. Yields of dust in the least massive
winds increase by a factor four when drift is used. We find drift velocities in
the range 10-67 km/s, which is drastically higher than in our earlier works
that use grey radiative transfer. It is necessary to include an estimate of
drift velocities to reproduce high yields of dust and low wind velocities.
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