| Abstract: Small-scale vortex flows in the solar photosphere are efficient drivers of magnetohydrodynamic (MHD) waves and are thought to play a significant role in transporting energy into the chromosphere. In this study, we employ three-dimensional radiative MHD simulations using the MURaM code to investigate the excitation, propagation, and evolution of torsional Alfvén waves generated by photospheric vortex motions within magnetic flux concentrations. The simulations provide a realistic treatment of convection, radiative transfer, and magnetic field dynamics, allowing us to identify rotational motions and quantify the resulting Alfvénic energy flux as it propagates upward into the chromosphere.
To enable direct comparison with observations, we perform forward modelling of chromospheric spectral lines, such as Ca II 854.2 nm, based on the simulation outputs. Synthetic observables—including intensity, Doppler velocity, and non-thermal line broadening—are analyzed to identify characteristic signatures of torsional wave motions. By linking vortex-driven torsional Alfvén waves in realistic numerical simulations to their observable chromospheric manifestations, this work aims to establish robust diagnostics for detecting Alfvénic wave activity and to assess their contribution to chromospheric energy transport and heating. |
