Department of Mathematics, Physics and Electrical Engineering, Northumbria University, Newcastle upon Tyne, UK
Natural Sciences (Astrophysics and Astrononmy)
The corona is known to be replete with Alfvénic waves. These highly incompressible transverse oscillations are potential candidates to heat the solar corona as well as accelerating the solar wind particles. A possible mechanism for effective dissipation of Alfvénic waves is turbulence, a process through which energy cascades down to smaller scales where it can be dissipated efficiently by resistivity or diffusivity. To date, two main populations of Alfvénic modes in the corona have been identified namely, decayless standing modes and propagating modes. A intriguing observational fact is that Active Region (AR) loops show standing Alfvénic oscillations, while Quiet Sun (QS) loops show only propagating Alfvénic waves. We go beyond previous studies of MHD wave turbulence in coronal loops by u
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