Study of AGB Mass Loss Models

Details Study of AGB Mass Loss Models Study of AGB Mass Loss Models

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21924006w&link_type=abstract

American Astronomical Society, AAS Meeting #219, #240.06

Astronomy and Astrophysics

Astronomy

Scientific paper

Stars that have reached the tip of the asymptotic giant branch (AGB) are as large and luminous as they can ever be. The mass loss time scale is shorter than the luminosity evolution time scale for mass loss rates exceeding 5x10-6(M/MSun) solar masses/year. At the same time the mass outflow is visible to observers since the column density is high. We are using the Bowen code to test the effects on mass loss rates and atmospheric structure of many stellar parameters, such as metallicity, luminosity and radius (related via mixing length), atmosphere opacity, dust condensation temperature, C/O ratio, driving amplitude, and non-LTE onset density. With this code it is possible to run a very large grid of models and look for the dependence of mass loss rate on stellar parameters and physical processes.

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