to stellar EPs within the disk, assumed to be a slab, has been modelled in @Rab.etal:17 who also assumed a rectilinear transport of particles within the circumstellar environment. Under the assumption that the EPs propagation is purely diffusive/advective, @Rodgers-Lee.etal:17 solved the transport equation and found that EPs dominate the disk ionisation only beyond $0.3$ AU, finding that they dilute with the distance from the star, $r$, as $r^{-1}$, whereas stellar $X$-rays simply dilute as $r^{-2}$.

In this paper, we examine the propagation of EPs in the environment of T Tauri stars with no assumption on diffusive motion. We adopt a magnetosphere, wind and extended magnetic field structure computed using a state-of-the-art MHD model commonly applied to the solar wind, and recently applied to study the winds and magnetospheres of other stars. We apply a particle transport model honed to model SEP propagation within the solar system to the magnetized, turbulent medium of the model T Tauri wind. We examine the predicted ionization rate as a function of radial distance and compare the results with the baseline TD09 study.

T TAURI WIND AND MAGNETOSPHERIC MODEL {#s:windmod}
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As our test case, we adopt one of the wind and magnetosphere models computed 