Speaker
Description
Solar wind energisation and acceleration have been long-standing problems in solar physics. Oftentimes, the possibility of magnetohydrodynamic (MHD) wave energy dissipation is invoked and explored in order to understand the physical processes behind these phenomena. The ubiquitous presence of MHD waves in the solar wind has been established through various in situ and remote observations. For example, MHD waves are known to manifest as incompressible Alfvénic fluctuations inside switchbacks, kink waves in flux tubes and in extended systems, and as wavelike signatures in coronagraphic observations. Using MHD modelling in an extended solar atmosphere, we study wave propagation and evolution along open and closed-field regions such as coronal holes and helmet streamers, respectively. The model includes important physics such as spherical expansion, gravitational stratification, thermal conduction, radiative cooling, and a background wind that transitions from being sub-Alfvénic to super-Alfvénic, in order to investigate wave reflection and trapping in different parts of the solar wind. We track the wave dynamics, the formation of small scales, and wave energy dissipation that feeds the solar wind as a wave front propagates out from the Sun. Our model aims to provide context to in situ and/or remote observations as well as to put forward theoretical constraints. This provides a deeper insight towards the understanding of the coupling mechanisms between MHD waves and the solar wind, particularly in the upper corona, where the solar wind is believed to be generated and accelerated.
| Do you plan to attend in-person or online? | In-person |
|---|
