2014/02/18 by R. Lionello, Roberto Lionello, Marco Velli +7 · 1 citation
Computer Science · Energy · Engineering · Physics and Astronomy · #Aerospace engineering #Atmospheric sciences #Engineering #Environmental science #Meteorology #Photovoltaic System Optimization Techniques #Physics #Plasma #Solar Radiation and Photovoltaics #Solar and Space Plasma Dynamics #Solar wind #Turbulence #astro-ph.SR
paper · pdf · doi:10.1088/0004-637x/784/2/120
arxiv created 2014/02/18 · openalex publication_date 2014/03/12 · arxiv updated 2015/06/18 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Although the mechanisms responsible for heating the Sun's corona and accelerating the solar wind are still being actively investigated, it is largely accepted that photospheric motions provide the energy source and that the magnetic field must play a key role in the process. Verdini et al. presented a model for heating and accelerating the solar wind based on the turbulent dissipation of Alfvén waves. We first use a time-dependent model of the solar wind to reproduce one of Verdini et al.'s solutions; then, we extend its application to the case where the energy equation includes thermal conduction and radiation losses, and the upper chromosphere is part of the computational domain. Using this model, we explore the parameter space and describe the characteristics of a fast solar wind solution. We discuss how this formulation may be applied to a three-dimensional MHD model of the corona and solar wind.