by @Drake.etal:17 for examining the shielding of cosmic rays by the stellar magnetic field and wind. We refer the reader to that work for further details and describe the model here only in brief.

The T Tauri wind model employed a recent version of the BATS-R-US Magnetohydrodynamics (MHD) code originally developed for the solar corona [@Powell.etal:99] as part of the Space Weather Modeling Framework [@Toth.etal:05; @Toth:12]. The model is based on Alfvén wave dissipation and couples, in a single simulation, the coronal thermodynamics and the solar wind acceleration in a self-consistent manner [@Sokolov.etal:13; @Oran.etal:13; @vanderHolst:14]. When applied to the solar case, the model employs high resolution magnetograms as a basis for the lower chromospheric magnetic field that drives the coronal heating and wind acceleration. @Drake.etal:17 used a surface magnetogram based on that constructed for the classical T Tauri star V2129 Oph from Zeeman-Doppler imaging by @Donati.etal:07. V2129 Oph is a typical T Tauri star, with an age of about 2 Myr, a mass of $1.35 M_\odot$, a radius of $2.4 R_\odot$, a rotation period of 6.53 d, and an accretion rate of $\sim 10^{-8}M_\odot$ yr$^{-1}$ [@Donati.etal:07]. @Drake.etal:17 employed different rotation periods in their models to examine its influence on cosmic 