  Alfv\'en-wave-driven 3D magnetohydrodynamic (MHD) models, which are
increasingly used to predict stellar wind properties, contain unconstrained
parameters and rely on low-resolution stellar magnetograms. We explore the
effects of the input Alfv\'en wave energy flux and the surface magnetogram on
the wind properties predicted by the Alfv\'en Wave Solar Model (AWSoM). We
lowered the resolution of two solar magnetograms during solar cycle maximum and
minimum using spherical harmonic decomposition. The Alfv\'en wave energy was
altered based on non-thermal velocities determined from a far ultraviolet (FUV)
spectrum of the solar twin 18 Sco. Additionally, low-resolution magnetograms of
three solar analogues were obtained using Zeeman Doppler imaging (ZDI).
Finally, the simulated wind properties were compared to Advanced Composition
Explorer (ACE) observations. AWSoM simulations using well constrained input
parameters taken from solar observations can reproduce the observed solar wind
mass and angular momentum loss rates. The resolution of the magnetogram has a
small impact on the wind properties and only during cycle maximum. However,
variation in Alfv\'en wave energy influences the wind properties irrespective
of the solar cycle activity level. Furthermore, solar wind simulations carried
out using the low-resolution magnetogram of the three stars instead of the
solar magnetogram could lead to an order of a magnitude difference in the
simulated wind properties. The choice in Alfv\'en energy has a stronger
influence on the wind output compared to the magnetogram resolution. The
influence could be even stronger for stars whose input boundary conditions are
not as well constrained as those of the Sun. Unsurprisingly, replacing the
solar magnetogram with a stellar magnetogram could lead to completely
inaccurate solar wind properties, and should be avoided in solar and stellar
wind simulations.
