Winds of M-type AGB stars driven by micron-sized grains

166 citations recorded by the source corpus.

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

Dust formation in the oxygen-rich AGB star IK Tauri (2015, background): “…that the growth of dust grains proceeds through surface deposition of atoms and molecules, and the final size of grains is controlled by accretion and evaporation under equilibrium conditions (Gail & Sedlmayr 1999; Ferraroti & Gail 2002; 2006; Woitke 2006; Höfner 2008; Dell’Agli et al. 2014).”
Production of dust by massive stars at high redshift (2011, background): “Höfner (2008) and Mattsson and Höfner (2011) have shown that larger grains of sizes in a very narrow range around 1µm can drive a wind.”
Mass loss of stars on the asymptotic giant branch (2018, methodology): “In these models, the outflows are driven by scattering of stellar photons on Fe-free silicate grains with radii in the range of 0.1–1µm, building on the results of Höfner (2008).”
Astrophysics with Extraterrestrial Materials (2016, background): “Models of dust formation in circumstellar outflows (e.g., Gail & Sedlmayr 1999, Höfner 2008) predict the specific phases that form and their properties (size, degree of crystallinity, etc.).”
Luminosities and mass-loss rates of SMC and LMC AGB stars and red supergiants (2009, unknown): “Höfner (2008) recently studied the winds of M giants using a ynamical atmosphere and wind models and concluded that ra- diation pressure is sufficient to drive the outflow if the restriction of small particles is relaxed.”