Fig. 4.
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Time variation during the AGB phase of the luminosity (left panel), mass-loss rate (middle), and pulsation period (right) of solar metallicity, model stars of initial mass 5 M⊙, in which mass loss was modelled according to Blo95 (black lines) and to VW93, where the scattering parameter β was set to 1 (green lines) and 3 (red).
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