  Constraining the processes that drive coronal heating from observations is a
difficult task due to the complexity of the solar atmosphere. As upcoming
missions such as MUSE will provide coronal observations with unprecedented
spatial and temporal resolution, numerical simulations are becoming
increasingly realistic. Despite the availability of synthetic observations from
numerical models, line-of-sight effects and the complexity of the magnetic
topology in a realistic setup still complicate the prediction of signatures for
specific heating processes. 3D MHD simulations have shown that a significant
part of the Poynting flux injected into the solar atmosphere is carried by
small-scale motions, such as vortices driven by rotational flows inside
intergranular lanes. MHD waves excited by these vortices have been suggested to
play an important role in the energy transfer between different atmospheric
layers. Using synthetic spectroscopic data generated from a coronal loop model
incorporating realistic driving by magnetoconvection, we study whether
signatures of energy transport by vortices and eventual dissipation can be
identified with future missions such as MUSE.
