D. Wójcik, B. Kuźma, K. Murawski, A. K. Srivastava
Published 2019-06-05Version 1
With the use of our JOANNA code, which solves radiative equations for ion + electron and neutralfluids, we perform realistic 2.5D numerical simulations of plasma outflows associated with the solargranulation. These outflows exhibit physical quantities consistentto the order of magnitude with theobservational findings for mass and energy losses in the upper chromosphere, transition region andinner corona, and they may originate the fast solar wind.
Heating and Acceleration of the Fast Solar Wind by Alfvén Wave Turbulence
Solar Cycle Variations in the Elemental Abundance of Helium and Fractionation of Iron in the Fast Solar Wind - Indicators of an Evolving Energetic Release of Mass from the Lower Solar Atmosphere
The Spectroscopic Footprint of the Fast Solar Wind
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