  I suggest a theoretical quantitative definition for the termination of the
asymptotic giant branch (AGB) phase and the beginning of the post-AGB phase. I
suggest that the transition will be taken to occur when the ratio of the
dynamical time scale to the the envelope thermal time scale, Q, reaches its
maximum value. Time average values are used for the different quantities, as
the criterion does not refer to the short time-scale variations occurring on
the AGB and post-AGB, e.g., thermal pulses (helium shell flashes) and magnetic
activity. Along the entire AGB the value of Q increases, even when the star
starts to contract. Only when a rapid contraction starts does the value of Q
start to decrease. This criterion captures the essence of the transition from
the AGB to the post AGB phase, because Q is connected to the stellar effective
temperature, reaching its maximum value at T~4000-6000 K, it is related to the
mass loss properties, and it reaches its maximum value when rapid contraction
starts and envelope mass is very low.
