  We present Magnetohydrodynamic (MHD) simulations of the magnetic interactions
between a solar type star and short period hot Jupiter exoplanets, using the
publicly available MHD code PLUTO. It has been predicted that emission due to
magnetic interactions such as the electron cyclotron maser instability (ECMI)
will be observable. In our simulations, a planetary outflow, due to UV
evaporation of the exoplanets atmosphere, results in the build-up of
circumplanetary material. We predict the ECMI emission and determine that the
emission is prevented from escaping from the system. This is due to the
evaporated material leading to a high plasma frequency in the vicinity of the
planet, which inhibits the ECMI process.
