  Stellar winds govern the angular momentum evolution of solar-like stars
throughout their main-sequence lifetime. The efficiency of this process depends
on the geometry of the star's magnetic field. There has been a rapid increase
recently in the number of stars for which this geometry can be determined
through spectropolarimetry. We present a computationally efficient method to
determine the 3D geometry of the stellar wind and to estimate the mass loss
rate and angular momentum loss rate based on these observations. Using solar
magnetograms as examples, we quantify the extent to which the values obtained
are affected by the limited spatial resolution of stellar observations. We find
that for a typical stellar surface resolution of 20$^{\rm o}$-30$^{\rm o}$,
predicted wind speeds are within 5$\%$ of the value at full resolution. Mass
loss rates and angular momentum loss rates are within 5-20$\%$. In contrast,
the predicted X-ray emission measures can be under-estimated by 1-2 orders of
magnitude, and their rotational modulations by 10-20$\%$.
