Models of Masers in AGB Stars (original) (raw)

Astrophysics and Space Science Library, 2003

Abstract

Coupling maser models to dynamical stellar envelope models provides a new step towards the full understanding of the physics of mass-losing stars. Here, we describe how such numerical simulations of H2O and SiO maser emission yield maser variability and the proper motions of maser clumps during a stellar pulsation cycle. These calculations place important constraints on stellar models and provide new insights on the conditions leading to, and predominantly affecting, stellar maser emission. This work also constitutes the foundations towards our final goal: the development of dynamical models of AGB stars which calculate accurately and self-consistently the time-dependent intensity and location of SiO, H2O and OH maser emisson, in addition to the inclusion of time-dependent chemistry and dust formation. Such models will provide a "big picture" view of mass-losing stellar envelopes throughout their pulsation cycles.

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