  Modelling isolated rotating stars at any rotation rate is a challenge for the
next generation of stellar models. These models will couple dynamical aspects
of rotating stars, like angular momentum and chemicals transport, with
classical chemical evolution, gravitational contraction or mass-loss. Such
modelling needs to be achieved in two dimensions, combining the calculation of
the structure of the star, its mean flows and the time-evolution of the whole.
We present here a first step in this challenging programme. It leads to the
first self-consistent two-dimensional models of rotating stars in a steady
state generated by the ESTER code. In these models the structure (pressure,
density and temperature) and the flow fields are computed in a self-consistent
way allowing the prediction of the differential rotation and the associated
meridian circulation of the stars. After a presentation of the physical
properties of such models and the numerical methods at work, we give the first
grid of such models describing massive and intermediate-mass stars for a
selection of rotation rates up to 90% of the breakup angular velocity.
