  The aim of this work is to study the energy transport by means of MHD waves
propagating in quiet Sun magnetic topology from layers below the surface to the
corona. Upward propagating waves find obstacles, such as the equipartition
layer with plasma b=1 and the transition region, and get converted, reflected
and refracted. Understanding the mechanisms by which MHD waves can reach the
corona can give us information about the solar atmosphere and the magnetic
structures. We carry out two-dimensional numerical simulations of wave
propagation in a magnetic field structure that consists of two vertical flux
tubes separated by an arcade shaped magnetic field. This configuration contains
a null point in the corona, that significantly modifies the behaviour of the
waves. We describe in detail the wave propagation through the atmosphere under
different driving conditions. We also present the spatial distribution of the
mean acoustic and magnetic energy fluxes and the spatial distribution of the
dominant frequencies in the whole domain. We conclude that the energy reaches
the corona preferably along vertical magnetic fields, inside the flux tubes,
and it has an acoustic nature. Most of the magnetic energy keeps concentrated
below the transition region due to the refraction of the magnetic waves and the
continuous conversion of acoustic-like waves into fast magnetic waves in the
equipartition layer located in the photosphere. However, part of the magnetic
energy reaches the low corona when propagating in the region where the arcades
are located, but waves are sent back downwards to the lower atmosphere at the
null point surroundings. This phenomenon, together with the reflection and
refraction of waves in the TR and the lower turning point, act as a re-feeding
of the atmosphere. In the frequency distribution, we find that high frequency
waves can reach the corona outside the vertical flux tubes.
