The transport and propagation of Solar Energetic Particles (SEPs) and the connection between observations at 1 AU and coronal acceleration regions is a key component of predicting space weather and energetic particle fluxes at the Earth. Drifts and scattering within the Interplanetary Magnetic Field (IMF) have a significant effect on the connection between in-situ observations and the location of the parent active region at the Sun. We present 3-D full-orbit test particle simulations of solar protons, launched from within the solar corona and propagating within a Parker spiral IMF, modified to account for a smooth current sheet. We assess asymmetry of particle drifts due to solar magnetic field orientation and the magnitudes of current sheet drifts. We quantify the effects of current sheet thickness on propagation of SEPs with energies ranging from 10 to 400 MeV. We discuss the implications on forecasting strong SEP events near the Earth.