The theory of radiation-driven winds succeeded in describing terminal
velocities and mass loss rates of massive stars. However, for A-type
supergiants the standard m-CAK solution predicts values of mass loss and
terminal velocity higher than the observed values. Based on the existence of a
slow wind solution in fast rotating massive stars, we explore numerically the
parameter space of radiation-driven flows to search for new wind solutions in
slowly rotating stars, that could explain the origin of these discrepancies. We
solve the 1-D hydrodynamical equation of rotating radiation-driven winds at
different stellar latitudes and explore the influence of ionization's changes
throughout the wind in the velocity profile. We have found that for particular
sets of stellar and line-force parameters, a new slow solution exists over the
entire star when the rotational speed is slow or even zero. In the case of slow
rotating A-type supergiant stars the presence of this novel slow solution at
all latitudes leads to mass losses and wind terminal velocities which are in
agreement with the observed values. The theoretical Wind Momentum-Luminosity
Relationship derived with these slow solutions shows very good agreement with
the empirical relationship. In addition, the ratio between the terminal and
escape velocities, which provides a simple way to predict stellar wind energy
and momentum input into the interstellar medium, is also properly traced.Comment: 7 Pages, 3 figures, Astrophysical Journal, Accepte