  The Sun and other solar-type stars have magnetic fields that permeate their
interior and surface, extends through the interplanetary medium, and is the
main driver of stellar activity. Stellar magnetic activity affects physical
processes and conditions of the interplanetary medium and orbiting planets.
Coronal mass ejections (CMEs) are the most impacting of these phenomena in
near-Earth space weather, and consist of plasma clouds, with magnetic field,
ejected from the solar corona. Precisely predicting the trajectory of CMEs is
crucial in determining whether a CME will hit a planet and impact its
magnetosphere and atmosphere. Despite the rapid developments in the search for
stellar CMEs, their detection is still very incipient. In this work we aim to
better understand the propagation of CMEs by analysing the influence of initial
parameters on CME trajectories, such as position, velocities, and stellar
magnetic field's configuration. We reconstruct magnetograms for Kepler-63 (KIC
11554435) and Kepler-411 (KIC 11551692) from spot transit mapping, and use a
CME deflection model, ForeCAT, to simulate trajectories of hypothetical CMEs
launched into the interplanetary medium from Kepler-63 and Kepler-411. We apply
the same methodology to the Sun, for comparison. Our results show that in
general, deflections and rotations of CMEs decrease with their radial velocity,
and increase with ejection latitude. Moreover, magnetic fields stronger than
the Sun's, such as Kepler-63's, tend to cause greater CME deflections.
