Magnetohydrodynamic processes in the sun’s atmosphere

The Sun’s atmosphere is a dynamic and complex structuring of the magnetic field and plasma in its various coupled layers, where magnetohydrodynamic (MHD) processes play a crucial role.

This talk will delve into the fascinating ideas about origin and evolution of cool jet-like flows in the Sun’s atmosphere using MHD theory. Solar cool jet-like flows are high-velocity ejecta that are impulsive and collimated plasma motions along the magnetic field lines in the Sun’s atmosphere. 

Small-scale cool jets (T<0.1 MK) and associated plasma dynamics have been detected in multiwavelength observations taken from space and ground-based instruments. Their physics can be understood in depth by performing numerical modelling using the MHD theory. We describe our few extensive MHD models in ideal and non-ideal regimes of plasma that demonstrate the origin and evolution of these cool jets and associated plasma processes. 

Our findings are consistent with various observations of cool solar jets. These scientific findings clarify the intricate relationship between plasma flows and complex structuring of the magnetic field leading to the evolution of various triggering processes of these jets. This also provides clues on their significant role in energy and mass transport into the lower solar corona. Specifically, we address the formation of such cool jets and associated plasma dynamics using 2-D and 2.5-D MHD modelling using Alfvén pulses, pressure pulses and vertical velocity pulses. The triggering mechanism (driver), dynamical evolution, kinematics, and energetics of such cool jets-like flows in the solar atmosphere are investigated. The non-adiabatic conditions (e.g., thermal-conduction and radiative-cooling) specifically affect the jet propagation, mass-flux, and kinetic energy density.

Venue: Fulton G20