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In recent years, coronal loops have been the focus of studies related to thedamping of different magnetohydrodynamic (MHD) surface waves and theirconnection with coronal seismology and wave heating. For a better understandingof wave heating, we need to take into account the effects of differentdissipation coefficients such as resistivity and viscosity, the importance ofthe loop physical characteristics, and the ways gravity can factor into theevolution of these phenomena. We aim to map the sites of energy dissipationfrom transverse waves in coronal loops in the presence and absence ofgravitational stratification and to compare ideal, resistive, and viscous MHD.Using the PLUTO code, we performed 3D MHD simulations of kink waves in single,straight, density-enhanced coronal flux tubes of multiple temperatures. We seethe creation of spatially expanded Kelvin-Helmholtz eddies along the loop,which deform the initial monolithic loop profile. For the case of drivenoscillations, the Kelvin-Helmholtz instability develops despite physicaldissipation, unless very high values of shear viscosity are used. Energydissipation gets its highest values near the apex, but is present all along theloop. We observe an increased efficiency of wave heating once the kineticenergy saturates at the later stages of the simulation and a turbulent densityprofile has developed. The inclusion of gravity greatly alters the dynamicevolution of our systems and should not be ignored in future studies. Strongerphysical dissipation leads to stronger wave heating in our set-ups. Finally,once the kinetic energy of the oscillating loop starts saturating, all theexcess input energy turns into internal energy, resulting in more efficientwave heating.

Wave heating in gravitationally stratified coronal loops in the presence of resistivity and viscosity