  With the first light of COROT, the preparation of KEPLER and the future
helioseismology spatial projects such as GOLF-NG, a coherent picture of the
evolution of rotating stars from their birth to their death is needed. We
describe here the modelling of the macroscopic transport of angular momentum
and matter in stellar interiors that we have undertaken to reach this goal.
First, we recall in detail the dynamical processes that are driving these
mechanisms in rotating stars and the theoretical advances we have achieved.
Then, we present our new results of numerical simulations which allow us to
follow in 2D the secular hydrodynamics of rotating stars, assuming that
anisotropic turbulence enforces a shellular rotation law. Finally, we show how
this work is leading to a dynamical vision of the Hertzsprung-Russel diagram
with the support of asteroseismology and helioseismology, seismic observables
giving constraints on the modelling of the internal transport and mixing
processes. In conclusion, we present the different processes that should be
studied in the next future to improve our description of stellar radiation
zones.
