  In the framework of f(R) scalar-tensor cosmology, we use the Noether symmetry
approach to find the cosmological models consistent with the Noether symmetry.
We obtain the functions f(R) and H(a), or the corresponding differential
equations, according to specific choices for the scalar field potential
V(\phi), the Brans-Dicke function \omega(\phi), some cosmological parameters,
and the constants of motion.
