Time Dependent Modelling of Mass Loss on the AGB
Previous numerical hydrodynamics calculations (Simis et al. 2001) indicated that the concentric shells around post-AGB objects and Planetary Nebulae may form due to an instability in the AGB wind. In this presentation I show the results of a series of calculations for various stellar parameters (T*, L*) that should enable to determine when this instability takes place. Also, I present first results of calculations that follow the outflow on a timescale longer than that of the mass loss modulation (which is typically of the order of a hundred years). This enables to study the effect of stellar evolution on the wind
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