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We present a new insight into the propagation, attenuation and dissipation oftwo-fluid, torsional Alfv\'en waves in the context of heating of the lowersolar atmosphere. By means of numerical simulations of the partially-ionizedplasma, we solve the set of two-fluid equations for ion plus electron andneutral fluids in three-dimensional (3D) Cartesian geometry. We implementinitially a current-free magnetic field configuration, corresponding to amagnetic flux-tube that is rooted in the solar photosphere and expands into thechromosphere and corona. We put the lower boundary of our simulation region inthe low chromosphere, where ions and neutrals begin to decouple, and implementthere a monochromatic driver that directly generates Alfv\'en waves with a waveperiod of 30 s. As the ion-neutral drift increases with height, the two-fluideffects become more significant and the energy carried by both Alfv\'en andmagneto-acoustic waves can be thermalized in the process of ion-neutralcollisions there. In fact, we observe a significant increase in plasmatemperature along the magnetic flux-tube. In conclusion, the two-fluidtorsional Alfv\'en waves can potentially play a role in the heating of thesolar chromosphere.

3D numerical simulations of propagating two-fluid, torsional Alfv\'en waves and heating of a partially-ionized solar chromosphere