  The study of the interaction between solid objects and magnetohydrodynamic
(MHD) fluids is of great importance in physics as consequence of the
significant phenomena generated, such as planets interacting with stellar wind
produced by their host stars. There are several computational tools created to
simulate hydrodynamic and MHD fluids, such as the FLASH code. In this code
there is a feature which permits the placement of rigid bodies in the domain to
be simulated. However, it is available and tested for pure hydrodynamic cases
only. Our aim here is to adapt the existing resources of FLASH to enable the
placement of a rigid body in MHD scenarios and, with such a scheme, to produce
the simulation of a non-magnetized planet interacting with the stellar wind
produced by a sun-like star. Besides, we consider that the planet has no
significant atmosphere. We focus our analysis on the patterns of the density,
magnetic field and velocity around the planet, as well as the influence of the
viscosity on such patterns. At last, an improved methodological approach is
available to other interested users.
