In this talk, I will show our recent results on 3D simulations of coronal loops driven with transverse waves at the footpoints. We find that the transverse waves convert to turbulence via the Kelvin-Helmholtz instability (for standing waves) or uniturbulence (for propagating waves). The latter is turbulence generated from the interaction of the driven propagating waves with the counterpropagating waves which are generated in-situ because of the plasma structure. Both of these turbulence generation mechanisms lead to fully turbulent loops, which allow for efficient energy dissipation and heating.
|Publication status||Published - 14 Dec 2017|
|Event||AGU Fall Meeting 2017 - New Orleans, United States|
Duration: 11 Dec 2017 → 15 Dec 2017
|Conference||AGU Fall Meeting 2017|
|Period||11/12/17 → 15/12/17|