copious shocks propagating in front of coronal mass ejections (CMEs) emanating from the star. In addition, if the Sun serves as a guide, such shocks are likely to be strong thereby producing hard particle spectra [@vanNes.etal.84 e.g.] that can provide a source of ionization for the protoplanetary disk. An alternative process that can efficiently produce non-thermal particles (electrons) in the proximity of the Sun is generally accepted to be the solar flare, as confirmed by hard $X$-rays due to bremsstrahlung emission of accelerated electrons [@Holman.etal:11] and by microwave radiation due to gyrosynchrotron of trans-relativistic electrons spiralling in the coronal magnetic field [@White.etal:11]. In our simulations, we calculate the propagation of EPs only, allowing the aforementioned processes of acceleration to operate in tandem and to produce $\sim$ GeV protons at a variety of distances from the star; only the position of particle injection into the circumstellar medium ($R_s$) is prescribed.

Our simulations explore two separate [characteristics]{} of disk ionization by EPs: 1) the topology of the stellar large-scale magnetic field wrapped around the T Tauri star; 2) turbulent fluctuations on small scales. [Both combined]{} will provide a realistic picture of the propagation of the EPs in the circumstellar medium of a 