We study the predicted rotational evolution of solar-type stars from the
pre-main sequence to the solar age with 1D rotating evolutionary models
including physical ingredients. We computed rotating evolution models of
solar-type stars including an external stellar wind torque and internal
transport of angular momentum following the method of Maeder and Zahn with the
code STAREVOL. We explored different formalisms and prescriptions available
from the literature. We tested the predictions of the models against recent
rotational period data from extensive photometric surveys, lithium abundances
of solar-mass stars in young clusters, and the helioseismic rotation profile of
the Sun. We find a best-matching combination of prescriptions for both internal
transport and surface extraction of angular momentum. This combination provides
a very good fit to the observed evolution of rotational periods for solar-type
stars from early evolution to the age of the Sun. Additionally, we show that
fast rotators experience a stronger coupling between their radiative region and
the convective envelope. Regardless of the set of prescriptions, however, we
cannot simultaneously reproduce surface angular velocity and the internal
profile of the Sun or the evolution of lithium abundance. We confirm the idea
that additional transport mechanisms must occur in solar-type stars until they
reach the age of the Sun. Whether these processes are the same as those needed
to explain recent asteroseismic data in more advanced evolutionary phases is
still an open question.Comment: 16 pages, 16 figures, accepted for publication in A&