  The kinematic and Period-Luminosity-Colour distribution of O-rich Long-Period
Variable stars of the solar neighbourhood is interpreted in terms of pulsation
modes, masses and metallicities. It is first shown that, because of input
physics imperfections, the periods and mean colours derived from the existing
linear and nonlinear nonadiabatic models must significantly depart from the
actual behaviour of the stars. As a consequence systematic corrections have to
be applied, as a first approximation, to our linear model grid. These free
parameters, as well as the mixing length, are calibrated on the LPVs of the LMC
and of some globular clusters, assuming a mean mass of one solar mass for the
LMC Mira-like stars. Then, the masses and metallicities corresponding to the
four kinematic/photometric populations of local LPVs are evaluated. The
possibility of a varying mixing-length parameter is discussed and taken into
account.
