The galactic mass injection from cool stellar winds of the 1 to 2.5 M-circle dot stars in the solar neighbourhood

We have computed synthetic stellar samples and HR diagrams on the basis of a fine-meshed, consistent grid of evolution tracks for given IMF and SFR(t) . In order to model the galactic disk stellar component (single stars only) and to derive its IMF and apparent SFR(t), we selected the synthetic sampl e which is the best fit to the observed distribution of single stars in the solar neighbourhood HR diagram (complete for d < 50 pc, M-V <less than or equal to> 4, based on Hipparcos data). Most giants of this synthetic sample fall in the range of M-i = 1 to 2.5 M.. Stellar evolution on the tip-AGE h as been computed by adopting, time-step by time-step: the mass-loss rates p redicted by very detailed dust-driven, pulsating wind models for carbon-ric h stars. This mass-loss description causes the natural development of super winds. Their properties are in agreement with the range of measured masses and expansion velocities of PNe, i.e. a total mass of between 0.25 M. and 0 .65 M. has been ejected over the final 30 thousand years. For the preceedin g mass-loss on the AGE and RGB, we use a semi-empirical approach, i.e., a r e-calibrated Reimers mass-loss which yields an RGB mass-loss (for M* less t han or similar to M.) consistent with the formation of horizontal branch st ars. Combining these approaches, we obtain a consistent grid of mass-loss h istories in the mass range of M-i = 1 to 2.5 M.. BY increasing the number o f stars in our synthetic solar neighbourhood stellar sample by a factor of thousand, we have been able to compute a detailed, present-day, synthetic r eference sample of galactic disk RGB and AGE giant stars, together with the ir mass-loss. The results are in good agreement with observations of cool g iant stellar mass-loss, as well as with the estimated space density of carb on stars. Finally, we discuss the relative collective yields of the RGB, AG E and tip-AGE stellar mass-loss as contributions to the galactic disk mass re-injection.