  A one-dimensional turbulent convection model in the form of a time-dependent
diffusion equation for the turbulent energy is incorporated into our numerical
pulsation code.
  The effect of turbulent convection on the structural rearrangement of the
static equilibrium star is taken into account, and the linear eigenvalues
(periods and growth-rates) for the complete turbulent convective nonadiabatic
pulsations of the equilibrium models are calculated.
  The linearized code allows us to perform efficiently a systematic survey of
the stability of Cepheid models for a wide range of astrophysical parameters
(L, M, Teff) and the turbulent convective parameters.
  A sensitivity analysis of the properties of several sequences of Galactic
Cepheids is performed with the goal of using observational constraints, such as
the shape and location of the fundamental and first overtone instability
strips, to calibrate the turbulent convective input parameters. The locations
of the red and blue edges of the fundamental and first overtone instability
strips and the overall strip widths are largely determined by the parameters
that determine the mixing length, and strengths of the eddy viscosity and of
the convective flux. The remaining parameters can be used for fine-tuning
agreement with observations.
