  Close-in planets orbiting around low-mass stars are exposed to intense
energetic photon and particle radiation and harsh space weather. We have
modeled such conditions for Proxima Centauri b (Garraffo et al. 2016b), a rocky
planet orbiting in the habitable-zone of our closest neighboring star, finding
a stellar wind pressure three orders of magnitude higher than the solar wind
pressure on Earth. At that time, no Zeeman-Doppler observations of the surface
magnetic field distribution of Proxima Cen were available and a proxy from a
star with similar Rossby number to Proxima was used to drive the MHD model.
Recently, the first ZDI observation of Proxima Cen became available (Klein et
al. 2021). We have modeled Proxima b's space weather using this map and
compared it with the results from the proxy magnetogram. We also computed
models for a high-resolution synthetic magnetogram for Proxima b generated by a
state-of-the-art dynamo model. The resulting space weather conditions for these
three scenarios are similar with only small differences found between the
models based on the ZDI observed magnetogram and the proxy. We conclude that
our proxy magnetogram prescription based on Rossby number is valid, and
provides a simple way to estimate stellar magnetic flux distributions when no
direct observations are available. Comparison with models based on the
synthetic magnetogram show that the exact magnetogram details are not important
for predicting global space weather conditions of planets, reinforcing earlier
conclusions that the large-scale (low-order) field dominates, and that the
small-scale field does not have much influence on the ambient stellar wind.
